VISIT 59 updated: STIS slit widened. ----- Attempting Submission 2 (Sat Aug 27 06:24:43 GMT 2011) ----- STIS slit widened Classical T Tauri stars undergo magnetospheric accretion, power outflows, and possess the physical and chemical conditions in their disks to give rise to planet formation. Existing high resolution FUV spectra verify that this spectral region offers unique diagnostics of these processes, which have the potential to significantly advance our understanding of the interaction of a star and its accretion disk. To date the limited results are intriguing, with dramatic differences in kinematic structure in lines ranging from C IV to H2 among the few stars that have been observed. We propose to use HST/COS to survey the disks, outflows, and accretion (the DAO) of 26 CTTS and 6 WTTS in the FUV at high spectral resolution. A survey of this size is essential to establish how properties of accretion shocks, winds and disk irradiation depend on disk accretion rate. Specifically, our goals are to (1) measure the radiation from and understand the physical properties of the gas very near the accretion shock as a function of accretion rate using emission line profiles of hot lines (C IV, Si IV, N V, and He II); (2) measure the opacity, velocity, and temperature at the base of the outflow to constrain outflow models using wind absorption features; and (3) characterize the radiation incident on disks and protoplanetary atmospheres using H2 line and continuum emission and reconstructed bright Ly-alpha line emission.

Most targets: Orbit 1: COS acquisition G130M (2 wavelength settings, 2 FP POS each) Orbit 2: G160M (3 wavelength settings, 1 FP POS each) Orbit 3: STIS acquisition Short G430L Short G230L Remainder: E230M The COS acquisition is typically with MIRROR B/PSA. Several brighter targets use MIRROR A+BOA, and two faint targets use MIRROR A/PSA. The STIS acquisition is usually performed with the long-pass filter, but in the brighter cases we use the O II or O III filter. A few sources are STIS-only due to concern with the COS safety limits. We went with STIS for anything that was close. We also use STIS with TWA 3A so that the secondary is out of the slit. We are not obtaining arcs for our low-resolution STIS spectra. Wavelength calibration to a similar accuracy can be performed on the stellar spectrum, and we will provide the wavelength 0-point to the archive before the data is released to the public. We are obtaining arcs for all high-resolution STIS spectra. These arcs are typically 25s integrations at the end of the orbit, based on estimates from other phase II programs. However, this integration time should be adjusted according to the recommendation from STScI. EXPOSURE TIME CALCULATIONS: --------------------- COS BUFFER TIMES: The buffer time is much larger than the exposure times, based on IUE spectra and the COS ETC. However, Ly-alpha fluxes from IUE are somewhat unreliable. When an orbit is split into two exposures, the first exposure has a buffer time equal to of the exposure time -110s. Our G130M spectra typically have buffer times of order 500-800s as insurance against a wildly mistaken Ly-alpha flux. We made these tables for our exposure time calculations: COS ACQUISITION -------------- Star F(2500) MIRROR t(S/N=40) Brt Pix (ct/s) Source: ---------------------------------------------------------- GM Aur 6d-15 B 19 11.9 STIS G230L DM Tau 4d-15 B 28 7.9 STIS G230L LkCa 15 1d-15 B 82 2.7 STIS G230L DN Tau 1.5d-15 B 76 2.9 IUE IP Tau 5d-16 B 160 1.4 FUV/check V836 Tau 3d-16 A 27 8.2 Optical/poor AA Tau 2d-15 B 47 4.8 IUE DE Tau 5d-15 B 23 9.9 IUE HN Tau 5d-15 B 19 12 Optical/poor FM Tau 2d-15 B 47 4.7 IUE SU Aur 1.5d-14 A/BOA 75 2.9 IUE DK Tau 1.5d-15 B 62 3.6 IUE UX Tau A 1.d-15 B 50 4.5 IUE DR Tau 2d-14 A/BOA 81 2.7 IUE RW Aur 3.5d-14 A/BOA 34 6.6 IUE CS Cha 2d-15 B 35 6.3 IUE RECX 15 .... B 29 7.8 IUE Sz 102 4d-16? B 200 1.2 Optical/very poor RECX 11 .... B 29 7.8 Optical/poor HBC 427 5d-16 A 10 21 Optical/poor LkCa 4 5d-16 A 10 21 Optical/poor LkCa 19 3d-15 B 29 7.8 IUE TWA 2 2d-15 B 20 5.2 IUE TWA 7 3d-15 B 29 7.8 IUE SCH J0439 6d-17 A 145 1.5 Optical/poor RECX 1 .... B 29 7.8 Optical/poor STIS ACQUISITION Target Filter Flux t_exp (S/N=40) Source ----------------------------------------------------- Hen 3-600A: O II 3700 1e-14 19.5 Optical spectrum HN Tau F28X50LP V=13.1 0.03 Optical spectrum Gm Aur F28X50LP V=12.2 0.017 Optical spectrum DM Tau F28X50LP V=13.8 0.053 Optical spectrum LkCa 15 F28X50LP V=12.1 0.011 Optical spectrum DN Tau F28X50LP V=12.5 0.023 Photometry IP Tau F28X50LP V=13.0 0.037 Photometry V836 Tau F28X50LP V=13.2 0.037 Photometry AA Tau F28X50LP V=12.8 0.027 Photometry DE Tau F28X50LP V=13.1 0.015 Optical Spectrum FM Tau F28X50LP V=13.6 0.06 Optical Spectrum SU Aur O III 5000 V=9.4 0.59 Photometry DK Tau F28X50LP V=12.6 0.027 Photometry DR Tau O II 3700 5d-14 3.6 Photometry UX Tau A O III 5000 V=10.7 1.9 Photometry RW Aur O II 3700 V=10.3 1.4 Photometry CS Cha F28X50LP V=11.6 0.006 Photometry RECX 15 F28X50LP V=14.0 Photometry CV Cha O II 3700 B=12.0 Photometry PDS 66 O II 3700 B=11.3 2.0 Photometry Sz 102 F28X50LP B=15, V=17. 1.3s Optical Spectrum RECX 11: O III 5000 V=11.2 2.0 Photometry HBC 427: F28X50LP V=11.6 0.006 Photometry LkCa 4 F28X50LP V=12.4 0.013 Photometry LkCa 19 F28X50LP V=11.3 0.0046 Photometry TWA 2 O III 5000 V=11.0 1.6 Photometry TWA 7 O III 5000 V=11.0 1.6 Photometry AK Sco O II 3700 B=9.9 0.47 Photometry HD104237 O II 3700 B=6.8 0.027 Photometry Most positions, PM are from Ducourant et al. (2005), most of which seem to be from UCAC2. Annoyingly, a few targets have RA and DEC measured from slightly different epochs (typically within 2 years). KNOWN BINARIES: -------- TWA 3: 1.46 arcsec binary. TWA 3A is about 3 times brighter than TWA 3B at 3700 A (but similar fluxes at longer wavelengths), which is why we choose that filter for target acquisition. HN Tau: 3.11 arcsec binary, with the primary 15 times brighter than the secondary in the optical and UV. ***********DK Tau: 2.30 arsec binary. A is brighter in the optical by 0.4 mag, they are about the same in the UV. Given the separation, I think the target acquisition procedure should work, but feedback would be helpful here.********************* UX Tau: UX Tau B is 5.9 arcsec away and much fainter (3 magnitudes in the B-band). RW Aur: RW Aur BC (a 0.09 arcsec close binary) is 1.42 arcsec away from RW Aur A. RW Aur A is our primary target. RW Aur A is 3 times brighter than BC at red wavelengths and 10 times brighter shortward of 6000 A. CS Cha, AK Sco: spectroscopic binaries, unresolvable HD104237: much brighter than nearby companions TWA 2A: 5 arcsec companion, 2.5 mag. fainter in V. After submitting the proposal, we obtained near-IR observations of FK Ser that reveal the target to be a 0.75 arcsec binary system. This complicates our COS observations. We prefer to keep the target, changed to STIS long-slit orbits. We will use a wide slit to include both targets. We would like to place very mild orientation constraints so that the PA of the slit is at least 20 degrees from the PA of the system. IF POSSIBLE, FOR DK TAU, TWA 3A, FK SER, UX Tau, TWA 2A, and HN Tau, we would like to be able to adjust the slit width depending on the date of observation. At certain orientations, we could get the secondary star on the slit and get serendipitous science in our STIS orbits. We do not request specific orientations because the science is secondary. However, if it's possible to change the slit width to account for the orientation, that would be quite useful. COOL STARS 12 false 0.0 0.0 false false false true AVAILABLE STAR T TAURI STAR Position from Ducourant et al. 2005 UPDATED: 23/12/09 FUV data measured from STIS G140L spectrum COS ACQ: --------- B/PSA: 7.1 cts/s COS G130M: --------- C II 1335 flux: 3.6e-14 erg/cm2/s s => 0.015 cts/ Ly-alpha: 4.3e-14 => 0.007 cts/s Variability: ------------ 96 observations: U=13.60 +/- 0.29; full range: U=12.99 -14.26 (Grankin et al. 2007) COS G160M: -------- C IV flux: 1.7e-13 => 0.03 cts/s STIS ACQ: --------- B=13.4, V=12.2 F28x50LP: saturation in 2.5-7s J2000 J2000 STAR T TAURI STAR Position from Ducourant et al. 2005 UPDATED: 23/12/09 SPECTRA: dmtau_g140l.dat; dmtau_g230l.dat COS ACQ: -------- B/PSA, 7.9 cts/s in brightest pix G130M: -------- C II flux: 2.5e-14 erg/cm2/s brightest pix: 0.01 cts/s Ly-alpha flux: <2d-14 erg/cm2/s (measured from STIS G140L) G160M: ------ C IV flux: 6.2e-14 erg/cm2/s brightest pix: 0.01 cts/s STIS ACQ: -------- B=14.6, V=13.8 F28x50LP: saturation in 5-10s Variability: ---------- Grankin et al. (2007): 8 U-band measurements: 14.8 +/- 0.4 (2-sigma); full range: 14.2-15.6 STIS ACQ: F28x50LP, saturation in 8s J2000 J2000 STAR T TAURI STAR Position from Ducourant et al. 2005 UPDATED: 23/12/09 J2000 J2000 STAR T TAURI STAR Position from Ducourant et al. 2005 UPDATED: 23/12/09 Position updated: 28/09/2010, obtained from ACS/SBC FUV image FUV lines measured from ACS SBC PR130L NUV observations taken from Valenti's IUE PMS archive: datasets at http://www.astro.caltech.edu/~gregoryh/11616/safety dntau_pr130l.dat dntau_iue.dat (NUV only) Variability: 45 U-band observations by Grankin et al. (2007): U=14.02 +/- 0.34 (1 sigma error) Umax=13.26, Umin=14.79 Assume everything is a factor of 4 higher than listed below => in worst-case scenario, still 10 times below sensitivity limit for grating, 4 times below COS ACQ limits DN Tau: ------- G160M: C IV 1549 A flux: 4.2e-14 erg/cm2/s C IV count rate: 0.008 cts/s G130M: ------ C II 1335 A flux: 4.2e-14 erg/cm2/s C II count rate: 0.018 cts/s Ly-alpha estimate: 4.3e-14 erg/cm2/s (based on H-alpha flux of 4.3e-13 erg/cm2/s). Ly-alpha count rate: 0.006 cts/s Alternate method: use H-alpha flux directly with Av=0.25 and N(H I) => Lya-alpha flux of 7.2e-14 erg/cm2/s. With the COS ETC, I calculate 0.009 cts/s. COS ACQUISITION: --------------- MIRRORB: 2.3 cts/s in brightest pixel, S/N=40 requires 98s STIS ACQ: ---------- V=12.3, F28x50LP: 0.0089s => S/N=40; saturation in 1.85s-3s STIS G230L, brightest pixel of 0.82 cts/s @2797 A (Mg II), less than limit of 75 J2000 J2000 STAR T TAURI STAR Position from Ducourant et al. 2005 UPDATED: 23/12/09 ------------------- Position updated: 28/09/2010: taken from NUV ACS image, Hartigan et al. ******************************************** IP Tau -------- Variability: 21 U-band observations (Bouvier et al. 1993) U=15.18 +/- 0.28 Umax=14.67, Umin=15.89 Multiply all estimates below by 3 for worst-case scenario. spectra: ------ iptau_pr130m.dat iptaublue.dat gmaur_g230l.dat (divided by 3.5) plot: iptau_template.ps IP Tau has no IUE or STIS near-UV spectrum (it does have an ACS PR200L spectrum, which is somewhat difficult to reduce). I have used GM Aur as a template. The plot, iptau_template.ps, compares the GM Aur blue Palomar+NUV STIS spectra*, divided by a factor of 3.5, with the optical spectrum from IP Tau. The template GM Aur should be quite reliable. You can see that the two stars look quite similar. *the NUV and blue spectra of GM Aur were obtained non-simultaneously, but had very similar flux levels. COS ACQ ---------- MIRRORB: 2.3 cts/s; S/N=40 requires 125 s COS G130M: --------- C II 1335 flux: 2.2e-15 erg/cm2/s C II count rate: 0.0001 cts/s in brightest pixel H-alpha flux: 3.9e-13 erg/cm2/s Estimated Ly-alpha flux: 3.9e-14 erg/cm2/s (multiply H-alpha by 0.1) Alternate Ly-alpha flux: 6.5e-14 erg/cm2/s (from Av, N(H I)) Ly-alpha count rate: 0.0088 cts/s (based on higher Ly-alpha flux). The estimated Ly-alpha flux, though uncertain, is far below the brightness limit. COS G160M: -------- C IV 1549 flux: 2.8e-14 erg/cm2/s C IV count rate: 0.0019 cts/s STIS ACQ: --------- F28x50LP V=13.0; saturation in 4.9s STIS G230L: brightest pixel 1.2 cts/s @ 2796 A (Mg II) J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED: 23/12/09 V836 TAU: this object is the 2nd faintest in our sample, and it should be the easiest to evaluate for potential violations of the COS brightness limits. V836 Tau was barely detected in a STIS E140M spectrum, and is obviously safe for the FUV gratings. No Ly-alpha emission was detected. For the COS NUV acquisitions, V836 Tau has few U-band observations. However, the accretion is weak enough that the U-band emission is dominated by the photosphere, to the point that several studies, including Valenti et al. 1993, used it as a spectral template for a non-accretor. In three U-band observations, Grankin et al. (2008) measured U=16.0 +/- 0.2, consistent with a STIS G430L observation an unpublished ground-based U-band observation. In 171 B-band observations, Grankin et al. measured B=14.9 +/- 0.25 (1 standard deviation), with a full range from 14.43-15.62. Spectra: V836tau_e140m.dat, v836_g430l.dat COS Acquisition: ----------- PSA, MIRRORA: 3.3 cts/s in brightest pixel G130M: -------- Ly-alpha flux: not detected (STIS) C II: not detected (STIS) G160M: -------- C IV flux: 1.1e-14 (STIS) => 0.002 cts/s in brightest pixel J2000 J2000 STAR T TAURI STAR Position from Ducourant et al. 2005 UPDATED: 23/12/09 --------------- SPECTRA: aatau_iue.dat COS ACQ: ---------- B/PSA: 3.4 cts/s COS G130M: --------- Maximum Ly-alpha flux: 7.3e-13 erg/cm2/s => 0.099 cts/s in brightest pixel. Given the Av, likely to be much less. C II flux: 4.8e-14 erg/cm2/s => 0.02 cts/s in brightest pixel COS G160M: ---------- C IV flux: 8.7e-14 erg/cm2/s => 0.015 cts/s STIS ACQ: 4s to saturation (V=12.8) Variability: 128 U-band observations from Grankin et al. (2007) U=14.7 +/- 0.5; full range: 13.7-16.1 J2000 J2000 STAR T TAURI STAR Variability: ---------- 26 observations: U=13.76 +/- 0.19; full range: 13.5 - 14.1 (Bouvier et al. 1993) Parallax from Ducourant et al. 2005 UPDATED: 23/12/09 COS ACQ --------- Aperture: B/PSA Brightest pixel: 9.9 COS G130M ------ O I 1305 triplet flux: 5.5e-14 erg/cm2/s brightest pixel: 0.01 cts/s/pix ESTIMATED Ly-alpha flux: 3.1e-13 erg/cm2/s brightest pixel: 0.042 cts/s/pix COS G160M: ------- C IV flux: 7.1e-14 erg/cm2/s brightest pixel: 0.012 cts/s STIS ACQ: F28x50LP -------- R=11.4, V=13.1, B=14.4 saturation: between 3-5s S/N=230 J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED: 23/12/09 J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED: 23/12/09 Position updated: 28/09/2009: obtained from NUV image (Hartigan PI) ----------- Herbst et al. (1994): 9 U-band observations: U_avg=14.6, range=13.8-15.6. IUE observation obtained when U was about 15.1. fmtau_iue.dat: MIRRORB => 3.9 cts/s. If 2 mags higher, 24 cts/s is still below the 50 cts/s limit. (using TW Hya/10 as a template, 5 cts/s) G130M: O I, C II emission not detected in an ACS/SBC PR130L spectrum. Ly-alpha emission: based on H-alpha flux/10, we estimate 6.6e-14 erg/cm2/s, which would correspond to 0.089 cts/s. Given the non-detection of O I emission with ACS, it is unlikely that any Ly-alpha emission will be detected G160M: C IV flux of 1.6e-14 from ACS/SBC PR130L spectrum. Using TW Hya as a spectral template, we estimate 0.003 cts/s in the brightest pixel. J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED: 23/12/09 Variability: 572 observations U=10.47 +/-0.25; full range: 10.13 -11.72 (Grankin et al. 2007) COS ACQ: ---------- A/BOA : 3.0 cts/s in brightest pixel COS G130M: --------- No Ly-alpha detected (STIS G140L) O I flux: 1.4e-13 0.026 cts/s in brightest pixel COS G160M: --------- C IV flux: 2.4e-13 erg/cm2/s 0.04 cts/s in brightest pixel STIS ACQ: ------ filter: O III 5007 B=10.2 => saturation in 90s J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 Position: F330W, J8MS07IAQ UPDATED: 23/12/09 J2000 J2000 STAR T TAURI STAR Hipparcos position/proper motion RA/DEC from WFPC2/F606W image, U44M3101R UPDATED: 23/12/09 -------------- UX Tau is a K5+M2 binary, so all photometry and IUE observations include both stars. However, almost all of the U-band and UV flux is produced by the primary, so we can ignore the secondary. Variability: range of 10 in 5 IUE spectra. Grankin et al. (2007): 94 U-band spectra, U=13.02 +/- 0.72; full range of 12.2-15.2. NUV spectrum: uxtau_lp06978.dat FUV spectrum: uxtau_iue.dat UX Tau: brightest IUE observation is lp06978. S/N is poor at short wavelengths, so lkca15_g230l.dat was used as a template. lkca15_g230l x 4 for the ETC. This IUE spectrum was obtained when U was about 13.3, so variability could increase the count rate by about a factor of 3. MIRRORB: brightest pixel=4.8 cts/s for the brightest IUE spectrum. Multiplying by 3 yields a count rate of 15 cts/s, well below the 50 cts/s limit. FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s G160M: brightest line is C IV, flux=9.4e-14 erg/cm2/s. Using TW Hya as a template, brightest pixel is 0.016 cts/s J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED: 23/12/09 J2000 J2000 STAR T TAURI STAR Position measured from J8MSA9QKQ, ACS F330W Proper motion from Ducourant et al. (2005) UPDATED: 24/12/09 J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPADATED: 23/12/09 -------------- Position updated: 28/9/2010, from ACS/SBC image Spectra: cscha_iue.dat VARIABILITY: ---------- CS Cha is a CTTS with U-band emission dominated by accretion. The U-band variability should be similar to NUV and FUV variability. Covino et al. (1992) present UBVRI photometry. In 11 epochs, U=13.34 +/- 0.16, with a full range from 13.06 - 13.60 mag. Guenther & Emerson (1997) present a few H-alpha measurements showing a flux that changes by from min to max. by 1.6 over a short period (days). Similar variability was seen in Mg II emission in three IUE NUV spectra. To be conservative, I will multiply estimates by a factor of 4 rather than1.6. COS ACQ: ------- B/PSA: 4.4 cts/s in brightest pixel (accounting for variability, mulitply by 4 => 18 cts/pix, below the brightness limit). 51s => S/N=40 G160M: ------- C IV 1549 A flux: 1.0e-13 erg/cm2/s. Using TW Hya as a spectral template yields 0.017 cts/s, well below the threshold. G130M: ------ Neither C II nor O I was detected with IUE, with an upper limit of about 5e-14 erg/cm2/s. This upper limit translates to about 0.02 cts/s in the brightest pixel. The measured H-alpha flux by Guenther & Emerson (1997) is 1.2e-12 erg/cm2/s. Since CS Cha is associated with a molecular cloud, I multiply the H-alpha flux by 0.1 to estimate a Ly-alpha flux of 1.2e-13 erg/cm2/s. This yields 0.016 cts/s in the brightest pixel. Alternately, the extinction is Av=0.8 mag (Espaillat et al. 2007). If I conservatively use Av=0.5, apply log N(H I)=20.9, and scale the Ly-alpha flux from TW Hya by the ratio of H-alpha line fluxes, I get 0.009 cts/s in the brightest pixel. With either option, there's plenty of room below the brightness limit. STIS G230L: Mg II: 4.2 cts/s from IUE flux of 2.8e-13 erg/cm2/s and scaling STIS E230M spectrum of TW Hya (Mg II from TW Hya: 3.2e-12 erg/cm2/s). J2000 J2000 STAR T TAURI STAR PM based on other cluster members, should lead to errors in the position of <1 arcsec J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 Proper motion UPDATED: 23/12/09 ------------- C IV 1549 about 3 times weaker than TW Hya, other FUV lines are weaker than that. NUV flux is similar to TW Hya. E140M: 0.15 cts/s at 1217 A, by scaling TW Hya E140M spectrum. E230M: Brightest pixel about 0.6 cts/s at 2796 A (Mg II), by scaling TW Hya E230M spectrum to Mg II flux of 5e-12 erg/cm2/s VARIABILITY: In 7 IUE observations, the Mg II flux varied from 2.8e-12 erg/cm2/s to 7.1e-12 erg/cm2/s. Continuum fluctuations are similar J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED: 23/12/09 J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED: 23/12/09 ------------- AK Sco lines: roughly 2x fainter than TW Hya. STIS E140M: maximum local count rate of 0.2 cts/s at 1217, much less than max of 75 DATA: aksco_iue.dat STIS E230M, long-wavelength setting: maximum local count of 0.6 cts/s. STIS E230M: global count rate of 8000 cts/s, 3000 from source (<<200,000 limit) Variability: V ranges from 8.7-10 (Alencar et al. 2003). Herbst et al. (1994) indicates similar variability in U-band. I would have guessed the FUV variability to be much larger, but in three IUE observations the range in C IV fluxes is from 5-6 x10^-13 erg/cm2/s. O I 1305 and C II 1335 are a little more variable, but not much. The FUV emission is surprisingly stable for AK Sco. J2000 J2000 STAR T TAURI STAR PM from Mamajek et al. 2005 Position from ACS/SBC image: J9YJ10011 UPDATED: 23/12/09 TWA 3A: ------- Variability of 20-30% from U-band 6 unpublished U-band spectra. This is an older CTTS and not likely to be variable. Any significant variability would have already been noted in the literature, as the object is well-studied. COS ACQ: -------- B/PSA: 1.8 cts/s in brightest pixel COS G130M: ----------- C II: 1.5e-14 erg/cm2/s 0.006 cts/s in brightest pixel Ly-alpha: PREDICTED (NOT MEAUSURED) flux of 1.5e-12, based on H-alpha emission 0.20 cts/s in brightest pixel COS G160M: ------------ C IV flux: 5.6e-14 erg/cm2/s => 0.0096 cts/s in brightest pixel STIS ACQ: ------- flux of 7e-15 erg/cm2/s/A at 3800 A => 34 s J2000 J2000 STAR T TAURI STAR Mamajek et al. (2002) UPDATED: 23/12/09 -------------------- The observations of this target include two STIS echelle setups (E140M, E230M) and a STIS G230L observation. The G230L observation is the only one that is potentially dangerous. Based on an IUE observation, the expected count rate is 1/10 of the limit. This target is safe for STIS. Brightness limits: used: pds66_iue.dat, twhya_e230m.dat Mg II 2800 flux: 2.1e-12 erg/cm2/s STIS G230L Brightest pixel: 7.7 cts/s at Mg II 2800. STIS E230M brightest pixel: Using TW Hya as a template: => 0.6 cts/s E140M: ---------- C IV 1549 A flux: 1.1e-12 Split into two lines, 1 A FWHM: 0.011 cts/s in brightest pixel Ly-alpha: somewhat uncertain, but from IUE (including geocoronal): 0.024 cts/s in brightest pixel: far below limit of 75 cts/s VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. J2000 J2000 STAR T TAURI STAR UCAC2 J2000 J2000 STAR HERBIG AE/BE Ducourant et al. 2005 J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED 23/12/09 ------------------ HBC 427: a WTTS, see LkCa 19 for longer explanation of characteristics. Very similar to cool stars. spectra: ------- hbc427_g430l.dat (STIS G430L) hbc427_g140l.dat (STIS G140L) hd98800_iue.dat (IUE NUV) hd98800blue.dat (optical-blue spectrum) Variability, from Grankin et al. (2007): 27 U-band observations U=14.02 +/- 0.15 (1-sigma) Umin: 13.73, Umax=14.41 Worst-case scenario: multiply broadband emission by 1.9 COS ACQ: ------- MIRRORA: 16 cts/s This is calculated from the HD98800 IUE spectrum. The two spectra match up very well from 3200-5000 A, with HBC 427 being 15 times fainter than HD98800. The HBC 427 observation occurred when U=14.3 (rough estimate), so close to its faintest level. That makes the "worst-case" count rate 30 cts/s. G160M: -------- C IV flux: 1.2e-14 erg/cm2/s => 0.003 cts/s G130M: ------ C II flux: 5.0e-15 erg/cm2/s => 0.0025 cts/s Ly-alpha flux: 1.5e-15 erg/cm2/s (tentative detection) J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED 23/12/09 LkCa 4 is a WTTS. This is what I wrote for a different WTTS: -------- The WTTSs present a different case than the CTTSs, though with similar problems. They are non-accreting cool stars, and exhibit spectra similar to cool stars (AU Mic, AD Leo, Epsilon Eri, etc.). Many of these sort of spectra can be found at Tom Ayres's CoolCAT website: http://casa.colorado.edu/~ayres/CoolCAT/ Per usual, Ly-alpha is usually not straightforward. From a small sample of bright cool stars in CoolCAT Star Mg II flux Ly-alpha flux* Ratio 70 Oph: 6.5e-11 5.8e-12 0.089 Eps Eri: 7.4e-11 1.55e-11 0.21 36 Oph: 2.6e-11 4.8e-12 0.18 Xi1 Boo: 3.7e-11 6.6e-12 0.18 kap Cet: 2.6e-11 3.0e-12 0.12 61 Vir: 1.2e-11 6.7e-13 0.06 Alpha cen: 1.1e-9 5.3e-11 0.05 Chi1Ori 4.5e-11 4.9e-12 0.11 *fluxes in erg/cm2/s Based on these few numbers, I'll use a flux ratio of Ly-alpha/Mg II=0.2. For stars in the Taurus Molecular Cloud, the actual Ly-alpha flux should be far less because of N(H I) in our line of sight. The WTTSs in the TW Hya Association will not necessarily suffer from a significant flux reduction because it is an older association, far from molecular material. Thus, this investigation is most important for those objects. *for reference, for 70 Oph the Ly-alpha emission would be 3.55 cts/s in the brightest pixel for a COS G130M observation. -------------- VARIABILITY: 18 U-band observations by Grankin et al. 2008: U=15.1+\- 0.34 mag, min=14.4, max=15.8 278 B-band observations by Grankin et al. 2008: B=14.03 +\- 0.19 mag, min=13.66, max=14.66 From min to max is 2.5^1.4=3.6, so multiply all count rates by 4. --------------- Spectra: FUV: lkca4_g140l.dat NUV: none, using hd98800_iue.dat as a template. No GALEX observation. COS ACQUSITION, MIRROR A/PSA: ----------------- From optical spectra and photopmetry (B=10.3 for HD98800, B=14.03 for LkCa 4), LkCa 4 is 30-50 time fainter than HD98800 in the NUV, which corresponds to 7-12 cts/s. The optical spectrum (50 times fainter) was obtained at U=15.2. If LkCa 4 is at the bright end, the count rate increases to 14-24 cts/s. COS ACQ: MIRRORA: 4.6 cts/s (x4=19 cts/s, safe for a WTTS) COS G130M: ---------- J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED 23/12/09 -------------- An explanation of the method first, then discussion of LkCa 19 spectra following ********** ****************** The WTTSs present a different case than the CTTSs, though with similar problems. They are non-accreting cool stars, and exhibit spectra similar to cool stars (AU Mic, AD Leo, Epsilon Eri, etc.). Many of these sort of spectra can be found at Tom Ayres's CoolCAT website: http://casa.colorado.edu/~ayres/CoolCAT/ Per usual, Ly-alpha is usually not straightforward. From a small sample of bright cool stars in CoolCAT Star Mg II flux Ly-alpha flux* Ratio 70 Oph: 6.5e-11 5.8e-12 0.089 Eps Eri: 7.4e-11 1.55e-11 0.21 36 Oph: 2.6e-11 4.8e-12 0.18 Xi1 Boo: 3.7e-11 6.6e-12 0.18 kap Cet: 2.6e-11 3.0e-12 0.12 61 Vir: 1.2e-11 6.7e-13 0.06 Alpha cen: 1.1e-9 5.3e-11 0.05 Chi1Ori 4.5e-11 4.9e-12 0.11 *fluxes in erg/cm2/s Based on these few numbers, I'll use a flux ratio of Ly-alpha/Mg II=0.2. For stars in the Taurus Molecular Cloud, the actual Ly-alpha flux should be far less because of N(H I) in our line of sight. The WTTSs in the TW Hya Association will not necessarily suffer from a significant flux reduction because it is an older association, far from molecular material. Thus, this investigation is most important for those objects. *for reference, for 70 Oph the Ly-alpha emission would be 3.55 cts/s in the brightest pixel for a COS G130M observation. ************************** I used AU Mic as a spectral template for the high-resolution FUV spectrum of a cool star. TEMPLATE FUV SPECTRUM: AU Mic ---------- E140M spectrum: http://www.astro.caltech.edu/~gregoryh/11616/safety/aumic_e140m.dat Use AU Mic as a template, scaling by C IV 1550 A flux C IV flux: 3.8e-13 erg/cm2/s G160M: 0.10 cts/s C II flux: 2.2e-13 erg/cm2/s G130M: 0.11 cts/s (outside of Ly-alpha) ************************** LkCa 19 ------- IUE spectrum: http://www.astro.caltech.edu/~gregoryh/11616/safety/lkca19_iue.dat COS ACQ: MIRRORB/PSA: 4.6 cts/s, time for S/N=40 => 50s COS G130M: C II: marginal detection of 1.1e-14 erg/cm2/s => 0.006 cts/s Ly-alpha: Measured Mg II flux (IUE): 1.8e-13 erg/cm2/s estimated Ly-alpha flux: 3.6e-14 erg/cm2/s => 0.022 cts/s in brightest pixel This estimate for Ly-alpha emission does not include the higher N(H I) and extinction to LkCa 19 relative to the nearby cool stars. COS G160M: Masured C IV flux: 2.0e-14 erg/cm2/s => 0.005 cts/s in G160M VARIABILITY: Grankin et al. (2008): 61 U-band observations; U=12.54 +/- 0.07 (1-sigma); min-max=0.38 mag i.e., very little variability. Note that this method likely underestimates the amount of variability in the lines, but should be good for the broadband MIRROR images. STIS acquisition: F28x150LP filter: 0.005s for S/N=40; saturation in 0.95s J2000 J2000 STAR T TAURI STAR PM from Mamajek et al. 2005, Position/epoch from UCAC2 J2000 J2000 STAR T TAURI STAR PM from Mamajek et al. 2005 Position measured from HST/ACS SBC image J9RH02011 UPDATED: 23/12/09 UPDATED: 16/02/11 J2000 J2000 STAR T TAURI STAR POSITION FROM Slesnick et al. 2006 PM from ALK UPDATED 23/12/09 ------------ SCH J0439+2336: this is the faintest object in our sample, an accreting star at the brown dwarf limit. An ACS/SBC PR130L spectrum demonstrates that the star is also faint in the FUV. Though PR130L doesn't cover Ly-alpha, based on H-alpha emission any Ly-alpha flux is surely weak. To assess the NUV acquisition images, based on the U-band emission seen in ground-based spectrum, dividing the GM Aur STIS G230L by a factor of 70 is appropriate. The lack of variability measurements is the only problem. As far as I know, the star has only been observed in the optical by Slesnick et al. (2006) and Herczeg et al. (2008). The two observations are consistent with each other. However, with the estimated count rate of 2.2 cts/s in the brightest pixel for the PSA and MIRRORA, even a factor of 10 increase in the emission would result in a flux below the bright limit cutoff. SPECTRA: -schj0439+2336_optical.dat -schj0439+2336_pr130l.dat COS ACQ: -------- Divide gmaur_g230l.dat by 75: 2.2 cts/s in brightest pixel, PSA/MIRRORA G160M: ------ C IV flux: 1.2e-15 erg/cm2/s => 0.0002 cts/s in brightest pixel G130M: ------ C II flux: not detected Estimated Ly-alpha flux: 3.8e-15 => 5e-4 cts/s in brightest pixel STIS ACQ: saturation in 15-35s J2000 J2000 STAR T TAURI STAR Ducourant et al. 2005 UPDATED 23/12/09 J2000 J2000 STAR T TAURI STAR Variability in Grankin et al. (2008) 2MASS-J16274028-2422040 J2000 J2000 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORB COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 STIS/CCD Imaging No No F28X50OII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 STIS/CCD Imaging No No F28X50OII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/CCD Imaging No No F28X50OII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 STIS/CCD Imaging No No F28X50OII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/FUV-MAMA Spectroscopic No No E140M 1425 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1623 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/CCD Imaging No No F28X50OIII STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 STIS/NUV-MAMA Spectroscopic No No E230M 2707 STIS/NUV-MAMA Spectroscopic No No G230L 2376 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1282225028000 266.3301385804075 (Tic-Visit :proposal-id 11616 :visit-id "01" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:29:16.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 933296 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2968 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3060 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "01" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2950 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) false 3 3 B/PSA: 7.1 cts/s B/PSA: 7.1 cts/s COS G130M: --------- C II 1335 flux: 3.6e-14 erg/cm2/s s => 0.015 cts/ Ly-alpha: 4.3e-14 => 0.007 cts/s COS G130M: --------- C II 1335 flux: 3.6e-14 erg/cm2/s s => 0.015 cts/ Ly-alpha: 4.3e-14 => 0.007 cts/s COS G130M: --------- C II 1335 flux: 3.6e-14 erg/cm2/s s => 0.015 cts/ Ly-alpha: 4.3e-14 => 0.007 cts/s COS G130M: --------- C II 1335 flux: 3.6e-14 erg/cm2/s s => 0.015 cts/ Ly-alpha: 4.3e-14 => 0.007 cts/s COS G160M: -------- C IV flux: 1.7e-13 => 0.03 cts/s COS G160M: -------- C IV flux: 1.7e-13 => 0.03 cts/s COS G160M: -------- C IV flux: 1.7e-13 => 0.03 cts/s STIS ACQ: --------- B=13.4, V=12.2 F28x50LP: saturation in 2.5-7s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1282484863000 260.91181450943753 (Tic-Visit :proposal-id 11616 :visit-id "02" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:29:22.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 968112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "02" :obset-id "A2" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2941 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 88 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3034 :al-overhead-at-end 0 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "02" :orbit-number 4 :pcs-time 333 :si-vis-utilization 2924 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 4 4 COS ACQ: -------- B/PSA, 7.9 cts/s in brightest pix COS ACQ: -------- B/PSA, 7.9 cts/s in brightest pix G130M: -------- C II flux: 2.5e-14 erg/cm2/s brightest pix: 0.01 cts/s Ly-alpha flux: <2d-14 erg/cm2/s (measured from STIS G140L) G130M: -------- C II flux: 2.5e-14 erg/cm2/s brightest pix: 0.01 cts/s Ly-alpha flux: <2d-14 erg/cm2/s (measured from STIS G140L) G130M: -------- C II flux: 2.5e-14 erg/cm2/s brightest pix: 0.01 cts/s Ly-alpha flux: <2d-14 erg/cm2/s (measured from STIS G140L) G130M: -------- C II flux: 2.5e-14 erg/cm2/s brightest pix: 0.01 cts/s Ly-alpha flux: <2d-14 erg/cm2/s (measured from STIS G140L) G160M: ------ C IV flux: 6.2e-14 erg/cm2/s brightest pix: 0.01 cts/s G160M: ------ C IV flux: 6.2e-14 erg/cm2/s brightest pix: 0.01 cts/s G160M: ------ C IV flux: 6.2e-14 erg/cm2/s brightest pix: 0.01 cts/s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1265326325000 82.18216458720121 (Tic-Visit :proposal-id 11616 :visit-id "03" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:29:27.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 915888 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "03" :obset-id "A3" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2943 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3036 :al-overhead-at-end 0 :internal-dur-at-end 371 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "03" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2925 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 3 3 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1315666874000 261.48419296889136 (Tic-Visit :proposal-id 11616 :visit-id "04" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 11:13:54.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1263792 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "04" :obset-id "A4" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 78 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "04" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 88 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "04" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3026 :al-overhead-at-end 0 :internal-dur-at-end 409 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "04" :orbit-number 4 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 4 0 COS ACQ: -------- B/PSA: 2.9 cts/s Variability: 45 U-band observations by Grankin et al. (2007): U=14.02 +/- 0.34 (1 sigma error) Umax=13.26, Umin=14.79 Assume everything is a factor of 4 higher than listed below => in worst-case scenario, still 10 times below sensitivity limit for grating, 4 times below COS ACQ limits COS ACQ: -------- B/PSA: 2.9 cts/s Variability: 45 U-band observations by Grankin et al. (2007): U=14.02 +/- 0.34 (1 sigma error) Umax=13.26, Umin=14.79 Assume everything is a factor of 4 higher than listed below => in worst-case scenario, still 10 times below sensitivity limit for grating, 4 times below COS ACQ limits COS G130M: ---------- C II: 4.2e-14 erg/cm2/s brightest pixel: 0.018 cts/s ESTIMATED Ly-alpha flux: 4.3e-14 erg/cm2/s, method (1) Brightest pix: 0.006 cts/s ESTIMATED Ly-alpha flux: 7.2e-14 erg/cm2/s, method (2) Brightest pix: 0.009 cts/s method (1): divide H-alpha flux by 10 method (2): use H-alpha flux, Av, and N(H I) to estimate Ly-alpha flux COS G130M: ---------- C II: 4.2e-14 erg/cm2/s brightest pixel: 0.018 cts/s ESTIMATED Ly-alpha flux: 4.3e-14 erg/cm2/s, method (1) Brightest pix: 0.006 cts/s ESTIMATED Ly-alpha flux: 7.2e-14 erg/cm2/s, method (2) Brightest pix: 0.009 cts/s method (1): divide H-alpha flux by 10 method (2): use H-alpha flux, Av, and N(H I) to estimate Ly-alpha flux COS G130M: ---------- C II: 4.2e-14 erg/cm2/s brightest pixel: 0.018 cts/s ESTIMATED Ly-alpha flux: 4.3e-14 erg/cm2/s, method (1) Brightest pix: 0.006 cts/s ESTIMATED Ly-alpha flux: 7.2e-14 erg/cm2/s, method (2) Brightest pix: 0.009 cts/s method (1): divide H-alpha flux by 10 method (2): use H-alpha flux, Av, and N(H I) to estimate Ly-alpha flux COS G130M: ---------- C II: 4.2e-14 erg/cm2/s brightest pixel: 0.018 cts/s ESTIMATED Ly-alpha flux: 4.3e-14 erg/cm2/s, method (1) Brightest pix: 0.006 cts/s ESTIMATED Ly-alpha flux: 7.2e-14 erg/cm2/s, method (2) Brightest pix: 0.009 cts/s method (1): divide H-alpha flux by 10 method (2): use H-alpha flux, Av, and N(H I) to estimate Ly-alpha flux COS G160M: ---------- C IV Flux: 4.2e-14 erg/cm2/2 Brightest pix: 0.008 cts/s COS G160M: ---------- C IV Flux: 4.2e-14 erg/cm2/s Brightest pix: 0.008 cts/s COS G160M: ---------- C IV Flux: 4.2e-14 erg/cm2/s Brightest pix: 0.008 cts/s STIS ACQ: -------- V=12.5 F28x50LP: saturation in 3s brightest pixel: 0.82 ct/s @2797 A (Mg II), less than limit of 75 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1300692928000 78.62702195367478 (Tic-Visit :proposal-id 11616 :visit-id "05" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:29:34.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1228992 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "05" :obset-id "A5" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2924 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "05" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 107 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "05" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "05" :orbit-number 4 :pcs-time 333 :si-vis-utilization 2924 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) false 4 0 COS ACQ ---------- MIRRORB: 2.3 cts/s; S/N=40 requires 100 s Variability: 21 U-band observations (Bouvier et al. 1993) U=15.18 +/- 0.28 Umax=14.67, Umin=15.89 Multiply all estimates below by 3 for worst-case scenario. spectra: ------ iptau_pr130m.dat iptaublue.dat gmaur_g230l.dat (divided by 3.5) plot: iptau_template.ps IP Tau has no IUE or STIS near-UV spectrum (it does have an ACS PR200L spectrum, which is somewhat difficult to reduce). I have used GM Aur as a template. The plot, iptau_template.ps, compares the GM Aur blue Palomar+NUV STIS spectra*, divided by a factor of 3.5, with the optical spectrum from IP Tau. The template GM Aur should be quite reliable. You can see that the two stars look quite similar. *the NUV and blue spectra of GM Aur were obtained non-simultaneously, but had very similar flux levels. COS ACQ ---------- MIRRORB: 2.3 cts/s; S/N=40 requires 100 s Variability: 21 U-band observations (Bouvier et al. 1993) U=15.18 +/- 0.28 Umax=14.67, Umin=15.89 Multiply all estimates below by 3 for worst-case scenario. spectra: ------ iptau_pr130m.dat iptaublue.dat gmaur_g230l.dat (divided by 3.5) plot: iptau_template.ps IP Tau has no IUE or STIS near-UV spectrum (it does have an ACS PR200L spectrum, which is somewhat difficult to reduce). I have used GM Aur as a template. The plot, iptau_template.ps, compares the GM Aur blue Palomar+NUV STIS spectra*, divided by a factor of 3.5, with the optical spectrum from IP Tau. The template GM Aur should be quite reliable. You can see that the two stars look quite similar. *the NUV and blue spectra of GM Aur were obtained non-simultaneously, but had very similar flux levels. COS G160M: -------- COS G160M: -------- C IV 1549 flux: 2.8e-14 erg/cm2/s C IV count rate: 0.0019 cts/s COS G160M: -------- C IV 1549 flux: 2.8e-14 erg/cm2/s C IV count rate: 0.0019 cts/s COS G160M: -------- C IV 1549 flux: 2.8e-14 erg/cm2/s C IV count rate: 0.0019 cts/s COS G130M: --------- C II 1335 flux: 2.2e-15 erg/cm2/s C II count rate: 0.0001 cts/s in brightest pixel H-alpha flux: 3.9e-13 erg/cm2/s Estimated Ly-alpha flux: 3.9e-14 erg/cm2/s (multiply H-alpha by 0.1) Alternate Ly-alpha flux: 6.5e-14 erg/cm2/s (from Av, N(H I)) Ly-alpha count rate: 0.0088 cts/s (based on higher Ly-alpha flux). The estimated Ly-alpha flux, though uncertain, is far below the brightness limit. COS G130M: --------- C II 1335 flux: 2.2e-15 erg/cm2/s C II count rate: 0.0001 cts/s in brightest pixel H-alpha flux: 3.9e-13 erg/cm2/s Estimated Ly-alpha flux: 3.9e-14 erg/cm2/s (multiply H-alpha by 0.1) Alternate Ly-alpha flux: 6.5e-14 erg/cm2/s (from Av, N(H I)) Ly-alpha count rate: 0.0088 cts/s (based on higher Ly-alpha flux). The estimated Ly-alpha flux, though uncertain, is far below the brightness limit. COS G130M: --------- C II 1335 flux: 2.2e-15 erg/cm2/s C II count rate: 0.0001 cts/s in brightest pixel H-alpha flux: 3.9e-13 erg/cm2/s Estimated Ly-alpha flux: 3.9e-14 erg/cm2/s (multiply H-alpha by 0.1) Alternate Ly-alpha flux: 6.5e-14 erg/cm2/s (from Av, N(H I)) Ly-alpha count rate: 0.0088 cts/s (based on higher Ly-alpha flux). The estimated Ly-alpha flux, though uncertain, is far below the brightness limit. COS G130M: --------- C II 1335 flux: 2.2e-15 erg/cm2/s C II count rate: 0.0001 cts/s in brightest pixel H-alpha flux: 3.9e-13 erg/cm2/s Estimated Ly-alpha flux: 3.9e-14 erg/cm2/s (multiply H-alpha by 0.1) Alternate Ly-alpha flux: 6.5e-14 erg/cm2/s (from Av, N(H I)) Ly-alpha count rate: 0.0088 cts/s (based on higher Ly-alpha flux). The estimated Ly-alpha flux, though uncertain, is far below the brightness limit. STIS ACQ: --------- F28x50LP V=13.0; saturation in 4.9s STIS G230L: brightest pixel 1.2 cts/s@2797 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1296880257000 65.0 (Tic-Visit :proposal-id 11616 :visit-id "06" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 21:06:52.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1594240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "06" :obset-id "C6" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2924 :al-overhead-at-end 0 :internal-dur-at-end 107 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "06" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3034 :al-overhead-at-end 0 :internal-dur-at-end 97 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "06" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 107 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "06" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "06" :orbit-number 5 :pcs-time 333 :si-vis-utilization 2924 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) false 5 0 COS Acquisition: ----------- PSA, MIRRORA: 3.3 cts/s in brightest pixel COS Acquisition: ----------- PSA, MIRRORA: 3.3 cts/s in brightest pixel G160M: -------- C IV flux: 1.1e-14 (STIS) => 0.002 cts/s in brightest pixel G160M: -------- C IV flux: 1.1e-14 (STIS) => 0.002 cts/s in brightest pixel G160M: -------- C IV flux: 1.1e-14 (STIS) => 0.002 cts/s in brightest pixel G130M: -------- Ly-alpha flux: not detected (STIS) C II: not detected (STIS) G130M: -------- Ly-alpha flux: not detected (STIS) C II: not detected (STIS) G130M: -------- Ly-alpha flux: not detected (STIS) C II: not detected (STIS) G130M: -------- Ly-alpha flux: not detected (STIS) C II: not detected (STIS) V=13, K7V Kurucz model, F28x50LP: Saturation in 4.8s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1294343903000 85.0722955220574 (Tic-Visit :proposal-id 11616 :visit-id "07" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 21:17:56.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1672528 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "07" :obset-id "B7" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "07" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "07" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3026 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "07" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "07" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "07" :orbit-number 5 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 5 0 B/PSA: 4.8 cts/s B/PSA: 4.8 cts/s COS G160M: ---------- C IV flux: 8.7e-14 erg/cm2/s => 0.015 cts/s COS G160M: ---------- C IV flux: 8.7e-14 erg/cm2/s => 0.015 cts/s COS G160M: ---------- C IV flux: 8.7e-14 erg/cm2/s => 0.015 cts/s COS G130M: --------- Maximum Ly-alpha flux: 7.3e-13 erg/cm2/s => 0.099 cts/s in brightest pixel. Given the Av, likely to be much less. C II flux: 4.8e-14 erg/cm2/s => 0.02 cts/s in brightest pixel COS G130M: --------- Maximum Ly-alpha flux: 7.3e-13 erg/cm2/s => 0.099 cts/s in brightest pixel. Given the Av, likely to be much less. C II flux: 4.8e-14 erg/cm2/s => 0.02 cts/s in brightest pixel COS G130M: --------- Maximum Ly-alpha flux: 7.3e-13 erg/cm2/s => 0.099 cts/s in brightest pixel. Given the Av, likely to be much less. C II flux: 4.8e-14 erg/cm2/s => 0.02 cts/s in brightest pixel COS G130M: --------- Maximum Ly-alpha flux: 7.3e-13 erg/cm2/s => 0.099 cts/s in brightest pixel. Given the Av, likely to be much less. C II flux: 4.8e-14 erg/cm2/s => 0.02 cts/s in brightest pixel STIS ACQ: 4s to saturation (V=12.8) The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1282305478000 261.69122840236446 (Tic-Visit :proposal-id 11616 :visit-id "08" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:29:52.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 985472 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "08" :obset-id "A8" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "08" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2952 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "08" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "08" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2934 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) false 3 3 Aperture: B/PSA Brightest pixel: 9.9 Aperture: B/PSA Brightest pixel: 9.9 O I 1305 triplet flux: 5.5e-14 erg/cm2/s brightest pixel: 0.01 cts/s/pix Ly-alpha flux: 3.1e-13 erg/cm2/s brightest pixel: 0.042 cts/s/pix O I 1305 triplet flux: 5.5e-14 erg/cm2/s brightest pixel: 0.01 cts/s/pix Ly-alpha flux: 3.1e-13 erg/cm2/s brightest pixel: 0.042 cts/s/pix O I 1305 triplet flux: 5.5e-14 erg/cm2/s brightest pixel: 0.01 cts/s/pix Ly-alpha flux: 3.1e-13 erg/cm2/s brightest pixel: 0.042 cts/s/pix O I 1305 triplet flux: 5.5e-14 erg/cm2/s brightest pixel: 0.01 cts/s/pix Ly-alpha flux: 3.1e-13 erg/cm2/s brightest pixel: 0.042 cts/s/pix C IV flux: 7.1e-14 erg/cm2/s brightest pixel: 0.012 cts/s C IV flux: 7.1e-14 erg/cm2/s brightest pixel: 0.012 cts/s C IV flux: 7.1e-14 erg/cm2/s brightest pixel: 0.012 cts/s R=11.4, V=13.1, B=14.4 saturation: from 2-5s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1265804648000 80.23436760015261 (Tic-Visit :proposal-id 11616 :visit-id "09" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:30:00.0" :trans-errors '(:WARNINGS 5 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1133344 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "09" :obset-id "B9" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "09" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2942 :al-overhead-at-end 0 :internal-dur-at-end 78 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "09" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3034 :al-overhead-at-end 0 :internal-dur-at-end 97 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "09" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 126 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "09" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "09" :orbit-number 5 :pcs-time 333 :si-vis-utilization 2924 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 5 5 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. (Tic-Visit :proposal-id 11616 :visit-id "10" :proposal-version -1 :trans-version "20100505" :date "10-Dec-2010 18:23:22.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1602928 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "10" :obset-id "A0" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "10" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2923 :al-overhead-at-end 0 :internal-dur-at-end 97 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "10" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3034 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "10" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 107 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "10" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "10" :orbit-number 5 :pcs-time 241 :si-vis-utilization 3016 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) false 5 0 Herbst et al. (1994): 9 U-band observations: U_avg=14.6, range=13.8-15.6. IUE observation obtained when U was about 15.1. fmtau_iue.dat: MIRRORB => 3.9 cts/s. If 2 mags higher, 24 cts/s is still below the 50 cts/s limit. (using TW Hya/10 as a template, 5 cts/s) Herbst et al. (1994): 9 U-band observations: U_avg=14.6, range=13.8-15.6. IUE observation obtained when U was about 15.1. fmtau_iue.dat: MIRRORB => 3.9 cts/s. If 2 mags higher, 24 cts/s is still below the 50 cts/s limit. (using TW Hya/10 as a template, 5 cts/s) G160M: C IV flux of 1.6e-14 from ACS/SBC PR130L spectrum. Using TW Hya as a spectral template, we estimate 0.003 cts/s in the brightest pixel. G160M: C IV flux of 1.6e-14 from ACS/SBC PR130L spectrum. Using TW Hya as a spectral template, we estimate 0.003 cts/s in the brightest pixel. G160M: C IV flux of 1.6e-14 from ACS/SBC PR130L spectrum. Using TW Hya as a spectral template, we estimate 0.003 cts/s in the brightest pixel. G130M: O I, C II emission not detected in an ACS/SBC PR130L spectrum. Ly-alpha emission: based on H-alpha flux/10, we estimate 6.6e-14 erg/cm2/s, which would correspond to 0.089 cts/s. Given the non-detection of O I emission with ACS, it is unlikely that any Ly-alpha emission will be detected G130M: O I, C II emission not detected in an ACS/SBC PR130L spectrum. Ly-alpha emission: based on H-alpha flux/10, we estimate 6.6e-14 erg/cm2/s, which would correspond to 0.089 cts/s. Given the non-detection of O I emission with ACS, it is unlikely that any Ly-alpha emission will be detected G130M: O I, C II emission not detected in an ACS/SBC PR130L spectrum. Ly-alpha emission: based on H-alpha flux/10, we estimate 6.6e-14 erg/cm2/s, which would correspond to 0.089 cts/s. Given the non-detection of O I emission with ACS, it is unlikely that any Ly-alpha emission will be detected G130M: O I, C II emission not detected in an ACS/SBC PR130L spectrum. Ly-alpha emission: based on H-alpha flux/10, we estimate 6.6e-14 erg/cm2/s, which would correspond to 0.089 cts/s. Given the non-detection of O I emission with ACS, it is unlikely that any Ly-alpha emission will be detected V ranges from 13.7-14.7. 11s to saturation The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1301038143000 81.10760016763561 (Tic-Visit :proposal-id 11616 :visit-id "11" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:30:08.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1176800 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "11" :obset-id "B1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "11" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2967 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "11" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "11" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2950 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) false 3 3 COS ACQ: ---------- A/BOA : 3.0 cts/s in brightest pixel COS ACQ: ---------- A/BOA : 3.0 cts/s in brightest pixel COS G160M: --------- C IV flux: 2.4e-13 erg/cm2/s 0.04 cts/s in brightest pixel COS G160M: --------- C IV flux: 2.4e-13 erg/cm2/s 0.04 cts/s in brightest pixel COS G160M: --------- C IV flux: 2.4e-13 erg/cm2/s 0.04 cts/s in brightest pixel COS G130M: --------- No Ly-alpha detected (STIS G140L) O I flux: 1.4e-13 0.026 cts/s in brightest pixel COS G130M: --------- No Ly-alpha detected (STIS G140L) O I flux: 1.4e-13 0.026 cts/s in brightest pixel COS G130M: --------- No Ly-alpha detected (STIS G140L) O I flux: 1.4e-13 0.026 cts/s in brightest pixel COS G130M: --------- No Ly-alpha detected (STIS G140L) O I flux: 1.4e-13 0.026 cts/s in brightest pixel STIS ACQ: ------ filter: O III 5007 flux: 7e-13 erg/cm2/s/A at 5100 A => saturation in 90s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1265305028000 83.12370271523469 (Tic-Visit :proposal-id 11616 :visit-id "12" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:30:17.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 985472 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "12" :obset-id "B2" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "12" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2952 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "12" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3045 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "12" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2934 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) false 3 3 Timing link suitability includes constraints ([34 After 13 by 0.1 to 0.1 days]) The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1292158295000 92.93021012604282 (Tic-Visit :proposal-id 11616 :visit-id "13" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:21:06.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 756880 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "13" :obset-id "13" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "13" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "13" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3025 :al-overhead-at-end 0 :internal-dur-at-end 400 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 2 0 Variability: range of 10 in 5 IUE spectra. Grankin et al. (2007): 94 U-band spectra, U=13.02 +/- 0.72; full range of 12.2-15.2. NUV spectrum: uxtau_lp06978.dat UX Tau: brightest IUE observation is lp06978. S/N is poor at short wavelengths, so lkca15_g230l.dat was used as a template. lkca15_g230l x 4 for the ETC. This IUE spectrum was obtained when U was about 13.3, so variability could increase the count rate by about a factor of 3. MIRRORB: brightest pixel=4.8 cts/s for the brightest IUE spectrum. Multiplying by 3 yields a count rate of 15 cts/s, well below the 50 cts/s limit. Variability: range of 10 in 5 IUE spectra. Grankin et al. (2007): 94 U-band spectra, U=13.02 +/- 0.72; full range of 12.2-15.2. NUV spectrum: uxtau_lp06978.dat UX Tau: brightest IUE observation is lp06978. S/N is poor at short wavelengths, so lkca15_g230l.dat was used as a template. lkca15_g230l x 4 for the ETC. This IUE spectrum was obtained when U was about 13.3, so variability could increase the count rate by about a factor of 3. MIRRORB: brightest pixel=4.8 cts/s for the brightest IUE spectrum. Multiplying by 3 yields a count rate of 15 cts/s, well below the 50 cts/s limit. FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G160M: brightest line is C IV, flux=9.4e-14 erg/cm2/s. Using TW Hya as a template, brightest pixel is 0.016 cts/s FUV spectrum: uxtau_iue.dat G160M: brightest line is C IV, flux=9.4e-14 erg/cm2/s. Using TW Hya as a template, brightest pixel is 0.016 cts/s FUV spectrum: uxtau_iue.dat G160M: brightest line is C IV, flux=9.4e-14 erg/cm2/s. Using TW Hya as a template, brightest pixel is 0.016 cts/s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1266230125000 81.26704393780301 (Tic-Visit :proposal-id 11616 :visit-id "14" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:30:26.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 915904 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "14" :obset-id "14" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "14" :obset-id "A4" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "14" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2942 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "14" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 381 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "14" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2924 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 3 3 1301016085000 82.79651196772772 (Tic-Visit :proposal-id 11616 :visit-id "15" :proposal-version -1 :trans-version "20100505" :date "10-Dec-2010 18:24:38.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1220352 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "15" :obset-id "15" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "15" :obset-id "B5" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "15" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2940 :al-overhead-at-end 0 :internal-dur-at-end 78 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "15" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3052 :al-overhead-at-end 0 :internal-dur-at-end 371 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "15" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2942 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) false 3 0 G230L, 3360 chosen to avoid Mg II line on detector Brightest pixel: 0.7 cts/s Count rate in Stripes A,B: 744, 821 respectively S/N=40 in 1.1s. Both far below the brightness limits of 50 cts/pix/s, 30000 cts/stripe/s Variability: --------- If 1 mag fainter, S/N=40 in 4s. If 2.5 mag brighter, 8000 cts/s/stripe and 7 cts/s in brightest pixel Grating/wavelength setting selected to avoid Mg II; G230L/3360 A setting not available. 80 cts/stripe, brightest pixel=0.055 cts/s, S/N=40 in 20s Grating/wavelength setting selected to avoid Mg II, minimize switches between exposure 2 and 3 80 cts/stripe, brightest pixel=0.055 cts/s, S/N=40 in 9s Brightest pixel from rwaur_uvopt.dat: 5.0 cts/s Variability (Grankin et al. 2007) U=10.9 +/- 0.5 (1-sigma), full range of 9.5-12.6 in 254 observations input observation: U=12.1 NUV acquisition from IUE spectrum: 5.0 cts/s If U=10 => 34 cts/s (97% confidence) If U=9.5 => 50 cts/s (99% confidence that the count rate will be below this rate) ***In the event that U<9.5, the brightness violation would be minor. If this image is not obtained, the observations will still be usable because the acquisition was done with a dispersed light acquisition to prevent an extremely rare even from causing an orbit loss. The object would likely be too faint for a BOA/MIRRORB image*** OTHER OBJECTS IN PSA FIELD: ----------------------- An ACS HRC F330W image, J8MSA9QKQ, shows only RW Aur A and B. The next brightest object in the field is 1000 times fainted than RW Aur A and about 5000 times fainter than RW Aur A, which is saturated. Two ACS PR200L images of RW Aur were obtained in 2004: j8msa9011 and j8msa9021 (first short, second longer). The faint third object has an approximate NUV continuum flux of 1e-16 erg/cm2/s/A, about 3500 times fainter than RW Aur A. From this image, I estimate about 3 cts/s if this object falls onto the PSA/MIRRORA during the BOA/MIRRORA acquisition, within the brightness limits of COS. scaling twhya_e140m.dat --------- C IV flux from IUE PMS archive: 2.3e-13 erg/cm2/s By comparison with TW Hya, this line will yield 0.04 cts/s, much less than the 0.7 cts/s limit VARIABILITY: ----------- 7 FUV spectra of C IV from RW Aur (6 IUE+1 GHRS): average flux of 2.0e-13 erg/cm2/s, max=3.7e-13 erg/cm2/s (=> 0.1 cts/s, safe). If U=11.8 (about the level for the IUE observation), then U=9.8 => 0.7 cts/s, at the limit. From the Grankin et al. variability measurements, 3 of 254 U-band measurements were brighter than 9.9. This observation has a 99% chance of being below the brightness limit. scaling twhya_e140m.dat --------- C IV flux from IUE PMS archive: 2.3e-13 erg/cm2/s By comparison with TW Hya, this line will yield 0.04 cts/s, much less than the 0.7 cts/s limit VARIABILITY: ----------- 7 FUV spectra of C IV from RW Aur (6 IUE+1 GHRS): average flux of 2.0e-13 erg/cm2/s, max=3.7e-13 erg/cm2/s (=> 0.1 cts/s for the max, safe). If U=11.8 (about the level for the IUE observation), then U=9.8 => 0.7 cts/s, at the limit. From the Grankin et al. variability measurements, 3 of 254 U-band measurements were brighter than 9.9. This observation has a 99% chance of being below the brightness limit. scaling twhya_e140m.dat --------- C IV flux fom IUE PMS archive: 2.3e-13 erg/cm2/s By comparison with TW Hya, this line will yield 0.04 cts/s, much less than the 0.7 cts/s limit VARIABILITY: ----------- 7 FUV spectra of C IV from RW Aur (6 IUE+1 GHRS): average flux of 2.0e-13 erg/cm2/s, max=3.7e-13 erg/cm2/s (=> 0.1 cts/s, safe). If U=11.8 (about the level for the IUE observation), then U=9.8 => 0.7 cts/s, at the limit. From the Grankin et al. variability measurements, 3 of 254 U-band measurements were brighter than 9.9. This observation has a 99% chance of being below the brightness limit. scaling twhya_e140m.dat --------------------- O I flux from IUE PMS archive spectrum: 2.5e-13 erg/cm2/s By comparison with TW Hya, this triplet will yield 0.05 cts/s, much less than the 0.7 cts/s limit Ly-alpha: No Taurus star has come close to violating the brightness limit at Ly-alpha because the N(H I) column attenuates most of the Ly-alpha emission. White & Ghez estimate A_v=0.4 to RW Aur A. The H-alpha emission of 1e-11 erg/cm2/s would lead to a maximum Ly-alpha flux of 1.0e-12 ergs/cm2/s, or 0.14 cts/s in the brightest pixel. Given N(H I), it's highly likely that the count rate at Ly-alpha will be much lower than this. VARIABILITY: ----------- 5 FUV spectra of O I from RW Aur (all IUE): average flux of 2.8e-13 erg/cm2/s, max=4.9e-13 erg/cm2/s (=> 0.1 cts/s, safe). U-band/FUV variability analysis similar to that for C IV scaling twhya_e140m.dat --------------------- O I flux from IUE PMS archive spectrum: 2.5e-13 erg/cm2/s By comparison with TW Hya, this triplet will yield 0.05 cts/s, much less than the 0.7 cts/s limit Ly-alpha: No Taurus star has come close to violating the brightness limit at Ly-alpha because the N(H I) column attenuates most of the Ly-alpha emission. White & Ghez estimate A_v=0.4 to RW Aur A. The H-alpha emission of 1e-11 erg/cm2/s would lead to a maximum Ly-alpha flux of 1.0e-12 ergs/cm2/s, or 0.14 cts/s in the brightest pixel. Given N(H I), it's highly likely that the count rate at Ly-alpha will be much lower than this. VARIABILITY: ----------- 5 FUV spectra of O I from RW Aur (all IUE): average flux of 2.8e-13 erg/cm2/s, max=4.9e-13 erg/cm2/s (=> 0.1 cts/s, safe). U-band/FUV variability analysis similar to that for C IV scaling twhya_e140m.dat --------------------- O I flux from IUE PMS archive spectrum: 2.5e-13 erg/cm2/s By comparison with TW Hya, this triplet will yield 0.05 cts/s, much less than the 0.7 cts/s limit Ly-alpha: No Taurus star has come close to violating the brightness limit at Ly-alpha because the N(H I) column attenuates most of the Ly-alpha emission. White & Ghez estimate A_v=0.4 to RW Aur A. The H-alpha emission of 1e-11 erg/cm2/s would lead to a maximum Ly-alpha flux of 1.0e-12 ergs/cm2/s, or 0.14 cts/s in the brightest pixel. Given N(H I), it's highly likely that the count rate at Ly-alpha will be much lower than this. VARIABILITY: ----------- 5 FUV spectra of O I from RW Aur (all IUE): average flux of 2.8e-13 erg/cm2/s, max=4.9e-13 erg/cm2/s (=> 0.1 cts/s, safe). U-band/FUV variability analysis similar to that for C IV scaling twhya_e140m.dat --------------------- O I flux from IUE PMS archive spectrum: 2.5e-13 erg/cm2/s By comparison with TW Hya, this triplet will yield 0.05 cts/s, much less than the 0.7 cts/s limit Ly-alpha: No Taurus star has come close to violating the brightness limit at Ly-alpha because the N(H I) column attenuates most of the Ly-alpha emission. White & Ghez estimate A_v=0.4 to RW Aur A. The H-alpha emission of 1e-11 erg/cm2/s would lead to a maximum Ly-alpha flux of 1.0e-12 ergs/cm2/s, or 0.14 cts/s in the brightest pixel. Given N(H I), it's highly likely that the count rate at Ly-alpha will be much lower than this. VARIABILITY: ----------- 5 FUV spectra of O I from RW Aur (all IUE): average flux of 2.8e-13 erg/cm2/s, max=4.9e-13 erg/cm2/s (=> 0.1 cts/s, safe). U-band/FUV variability analysis similar to that for C IV from rwaur_nuvopt.dat: -------------- Time to S/N=40: 3.5s Time to saturation: 56s at 3200 A: S/N=24/resel brightest pixel (4860): 243 cts/s saturation in 135s S/N=15 at 1800 A Brightest pixel: 25 cts/s at 2800 A Brightest pixel: 1.35 cts/s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1306949139000 75.0 (Tic-Visit :proposal-id 11616 :visit-id "16" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:25:30.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1229056 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "16" :obset-id "16" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "16" :obset-id "A6" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "16" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3299 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "16" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3411 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "16" :orbit-number 3 :pcs-time 333 :si-vis-utilization 3300 :al-overhead-at-end 0 :internal-dur-at-end 802 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) false 3 0 Spectra: cscha_iue.dat VARIABILITY: ---------- CS Cha is a CTTS with U-band emission dominated by accretion. The U-band variability should be similar to NUV and FUV variability. Covino et al. (1992) present UBVRI photometry. In 11 epochs, U=13.34 +/- 0.16, with a full range from 13.06 - 13.60 mag. Guenther & Emerson (1997) present a few H-alpha measurements showing a flux that changes by from min to max. by 1.6 over a short period (days). Similar variability was seen in Mg II emission in three IUE NUV spectra. To be conservative, I will multiply estimates by a factor of 4 rather than1.6. COS ACQ: ------- B/PSA: 4.4 cts/s in brightest pixel (accounting for variability, mulitply by 4 => 18 cts/pix, below the brightness limit). 51s => S/N=40 Spectra: cscha_iue.dat VARIABILITY: ---------- CS Cha is a CTTS with U-band emission dominated by accretion. The U-band variability should be similar to NUV and FUV variability. Covino et al. (1992) present UBVRI photometry. In 11 epochs, U=13.34 +/- 0.16, with a full range from 13.06 - 13.60 mag. Guenther & Emerson (1997) present a few H-alpha measurements showing a flux that changes by from min to max. by 1.6 over a short period (days). Similar variability was seen in Mg II emission in three IUE NUV spectra. To be conservative, I will multiply estimates by a factor of 4 rather than1.6. COS ACQ: ------- B/PSA: 4.4 cts/s in brightest pixel (accounting for variability, mulitply by 4 => 18 cts/pix, below the brightness limit). 51s => S/N=40 G130M: ------ Neither C II nor O I was detected with IUE, with an upper limit of about 5e-14 erg/cm2/s. This upper limit translates to about 0.02 cts/s in the brightest pixel. The measured H-alpha flux by Guenther & Emerson (1997) is 1.2e-12 erg/cm2/s. Since CS Cha is associated with a molecular cloud, I multiply the H-alpha flux by 0.1 to estimate a Ly-alpha flux of 1.2e-13 erg/cm2/s. This yields 0.016 cts/s in the brightest pixel. Alternately, the extinction is Av=0.8 mag (Espaillat et al. 2007). If I conservatively use Av=0.5, apply log N(H I)=20.9, and scale the Ly-alpha flux from TW Hya by the ratio of H-alpha line fluxes, I get 0.009 cts/s in the brightest pixel. With either option, there's plenty of room below the brightness limit. G130M: ------ Neither C II nor O I was detected with IUE, with an upper limit of about 5e-14 erg/cm2/s. This upper limit translates to about 0.02 cts/s in the brightest pixel. The measured H-alpha flux by Guenther & Emerson (1997) is 1.2e-12 erg/cm2/s. Since CS Cha is associated with a molecular cloud, I multiply the H-alpha flux by 0.1 to estimate a Ly-alpha flux of 1.2e-13 erg/cm2/s. This yields 0.016 cts/s in the brightest pixel. Alternately, the extinction is Av=0.8 mag (Espaillat et al. 2007). If I conservatively use Av=0.5, apply log N(H I)=20.9, and scale the Ly-alpha flux from TW Hya by the ratio of H-alpha line fluxes, I get 0.009 cts/s in the brightest pixel. With either option, there's plenty of room below the brightness limit. G130M: ------ Neither C II nor O I was detected with IUE, with an upper limit of about 5e-14 erg/cm2/s. This upper limit translates to about 0.02 cts/s in the brightest pixel. The measured H-alpha flux by Guenther & Emerson (1997) is 1.2e-12 erg/cm2/s. Since CS Cha is associated with a molecular cloud, I multiply the H-alpha flux by 0.1 to estimate a Ly-alpha flux of 1.2e-13 erg/cm2/s. This yields 0.016 cts/s in the brightest pixel. Alternately, the extinction is Av=0.8 mag (Espaillat et al. 2007). If I conservatively use Av=0.5, apply log N(H I)=20.9, and scale the Ly-alpha flux from TW Hya by the ratio of H-alpha line fluxes, I get 0.009 cts/s in the brightest pixel. With either option, there's plenty of room below the brightness limit. G130M: ------ Neither C II nor O I was detected with IUE, with an upper limit of about 5e-14 erg/cm2/s. This upper limit translates to about 0.02 cts/s in the brightest pixel. The measured H-alpha flux by Guenther & Emerson (1997) is 1.2e-12 erg/cm2/s. Since CS Cha is associated with a molecular cloud, I multiply the H-alpha flux by 0.1 to estimate a Ly-alpha flux of 1.2e-13 erg/cm2/s. This yields 0.016 cts/s in the brightest pixel. Alternately, the extinction is Av=0.8 mag (Espaillat et al. 2007). If I conservatively use Av=0.5, apply log N(H I)=20.9, and scale the Ly-alpha flux from TW Hya by the ratio of H-alpha line fluxes, I get 0.009 cts/s in the brightest pixel. With either option, there's plenty of room below the brightness limit. G160M: ------- C IV 1549 A flux: 1.0e-13 erg/cm2/s. Using TW Hya as a spectral template yields 0.017 cts/s, well below the threshold. G160M: ------- C IV 1549 A flux: 1.0e-13 erg/cm2/s. Using TW Hya as a spectral template yields 0.017 cts/s, well below the threshold. G160M: ------- C IV 1549 A flux: 1.0e-13 erg/cm2/s. Using TW Hya as a spectral template yields 0.017 cts/s, well below the threshold. saturation in 1.5s STIS G230L: Mg II: 4.2 cts/s from IUE flux of 2.8e-13 erg/cm2/s and scaling STIS E230M spectrum of TW Hya (Mg II from TW Hya: 3.2e-12 erg/cm2/s). The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1265380375000 7.885056844058994 (Tic-Visit :proposal-id 11616 :visit-id "17" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:30:40.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1359424 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "17" :obset-id "17" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "17" :obset-id "C7" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "17" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3343 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "17" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3436 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "17" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3436 :al-overhead-at-end 0 :internal-dur-at-end 400 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "17" :orbit-number 4 :pcs-time 333 :si-vis-utilization 3325 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) false 4 4 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1302727118000 39.313526322484904 (Tic-Visit :proposal-id 11616 :visit-id "18" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:26:15.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1968144 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "18" :obset-id "18" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "18" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3325 :al-overhead-at-end 0 :internal-dur-at-end 325 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "18" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3436 :al-overhead-at-end 0 :internal-dur-at-end 325 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "18" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3436 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) false 3 3 0.006s => S/N=40 1.1s => saturation E230M: Brightest pixel about 0.6 cts/s at 2796 A (Mg II), by using TW Hya E230M spectrum and measured Mg II fluxes. VARIABILITY: In 7 IUE observations, the Mg II flux varied from 2.8e-12 erg/cm2/s to 7.1e-12 erg/cm2/s. C IV 1549 about 3 times weaker than TW Hya, other FUV lines are weaker than that. NUV flux is similar to TW Hya. Bright count rate for E140M: 0.15 cts/s at 1217 A, by scaling TW Hya E140M spectrum. C IV 1549 about 3 times weaker than TW Hya, other FUV lines are weaker than that. NUV flux is similar to TW Hya. Bright count rate for E140M: 0.15 cts/s at 1217 A, by scaling TW Hya E140M spectrum. The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1306688744000 355.0 (Tic-Visit :proposal-id 11616 :visit-id "19" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:26:25.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 846288 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "19" :obset-id "19" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "19" :obset-id "A9" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "19" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2993 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "19" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3086 :al-overhead-at-end 0 :internal-dur-at-end 409 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "19" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2977 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) false 3 3 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1282412744000 92.02871976007009 (Tic-Visit :proposal-id 11616 :visit-id "21" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:30:54.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 506960 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "21" :obset-id "21" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "21" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2977 :al-overhead-at-end 201 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "21" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3088 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) false 2 2 B=9.9 0.4s => S/N=40 52s => saturation 8000 cts/s detector; 3000 from source (limits=200,000) Brightest pixel: 0.63 cts/s (limit=75) from measured Mg II emission DATA: aksco_iue.dat Brightest pixel: 0.2 cts/s (<<75 cts/s) from ESTIMATE of Ly-alpha emission, based on simple scaling of TW Hya from other FUV lines. From IUE spectrum: the Ly-alpha flux is about 1.4e-11, or 0.3 times that of TW Hya, which would lead to a count rate of 0.15 cts/s. Both estimates above are unreliable, but are far below the brightness limits The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1301120063000 34.5 (Tic-Visit :proposal-id 11616 :visit-id "22" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:30:58.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 802608 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "22" :obset-id "22" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "22" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2977 :al-overhead-at-end 0 :internal-dur-at-end 540 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "22" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3088 :al-overhead-at-end 0 :internal-dur-at-end 480 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "22" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3088 :al-overhead-at-end 300 :internal-dur-at-end 134 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "22" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3088 :al-overhead-at-end 0 :internal-dur-at-end 801 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) false 4 4 STIS ACQ: ------- flux of 7e-15 erg/cm2/s/A at 3800 A => 34 s for S/N=40 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1306128534000 30.0 (Tic-Visit :proposal-id 11616 :visit-id "23" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:02.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 576448 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "23" :obset-id "23" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "23" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3281 :al-overhead-at-end 0 :internal-dur-at-end 540 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3599 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "23" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3392 :al-overhead-at-end 0 :internal-dur-at-end 540 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3599 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "23" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3392 :al-overhead-at-end 0 :internal-dur-at-end 802 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3599 :pcs-gap 0 ) false 3 3 V=10.35, time=1.4s for S/N=40 saturation=270s pds66_iue.dat Brightest pixel: 7.7 cts/s at Mg II. VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. Mg II 2800 flux: 2.1e-12 erg/cm2/s Using TW Hya as a template: => 0.6 cts/s VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. C IV 1549 A flux: 1.1e-12 Split into two lines, 1 A FWHM: 0.011 cts/s in brightest pixel Ly-alpha: somewhat uncertain, but from IUE (including geocoronal): 0.024 cts/s in brightest pixel: far below limit of 75 cts/s VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. C IV 1549 A flux: 1.1e-12 Split into two lines, 1 A FWHM: 0.011 cts/s in brightest pixel Ly-alpha: somewhat uncertain, but from IUE (including geocoronal): 0.024 cts/s in brightest pixel: far below limit of 75 cts/s VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. (Tic-Visit :proposal-id 11616 :visit-id "20" :proposal-version -1 :trans-version "20100505" :date "10-Dec-2010 16:55:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 924368 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "20" :obset-id "20" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "20" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 540 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "20" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 540 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "20" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3027 :al-overhead-at-end 0 :internal-dur-at-end 802 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 3 0 V=10.35, time=1.4s for S/N=40 saturation=270s pds66_iue.dat Brightest pixel: 7.7 cts/s at Mg II. VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. Mg II 2800 flux: 2.1e-12 erg/cm2/s Using TW Hya as a template: => 0.6 cts/s VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. C IV 1549 A flux: 1.1e-12 Split into two lines, 1 A FWHM: 0.011 cts/s in brightest pixel Ly-alpha: somewhat uncertain, but from IUE (including geocoronal): 0.024 cts/s in brightest pixel: far below limit of 75 cts/s VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. C IV 1549 A flux: 1.1e-12 Split into two lines, 1 A FWHM: 0.011 cts/s in brightest pixel Ly-alpha: somewhat uncertain, but from IUE (including geocoronal): 0.024 cts/s in brightest pixel: far below limit of 75 cts/s VARIABILITY: Batalha et al. indicate very little variability in the U-band for PDS 66 (standard deviation = 0.12 mag). It's an early-type star, so I would expect more variability than that in the lines. However, with fluxes 10 times lower than the STIS brightness limit for all observations, including the G230L, this object is safe. The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1260578626000 310.4161422112695 (Tic-Visit :proposal-id 11616 :visit-id "24" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:08.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1150688 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "24" :obset-id "24" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "24" :obset-id "B4" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "24" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3363 :al-overhead-at-end 0 :internal-dur-at-end 88 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "24" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3457 :al-overhead-at-end 0 :internal-dur-at-end 88 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "24" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3459 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "24" :orbit-number 4 :pcs-time 333 :si-vis-utilization 3325 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) false 4 4 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1259981131000 256.54178482090924 (Tic-Visit :proposal-id 11616 :visit-id "25" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:12.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1081056 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "25" :obset-id "25" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "25" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3325 :al-overhead-at-end 201 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "25" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3463 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) false 2 2 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1301440728000 80.48850719252158 (Tic-Visit :proposal-id 11616 :visit-id "26" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:27:36.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1220320 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "26" :obset-id "26" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "26" :obset-id "B6" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "26" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2968 :al-overhead-at-end 0 :internal-dur-at-end 107 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "26" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3061 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "26" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2950 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) false 3 3 COS ACQ: ------- Variability, from Grankin et al. (2007): 27 U-band observations U=14.02 +/- 0.15 (1-sigma) Umin: 13.73, Umax=14.41 Worst-case scenario: multiply broadband emission by 1.9 MIRRORA: 16 cts/s!! This is calculated from the HD98800 IUE spectrum. The two spectra match up very well from 3200-5000 A, with HBC 427 being 15 times fainter than HD98800. The HBC 427 observation occurred when U=14.3 (rough estimate), so close to its faintest level. That makes the "worst-case" count rate 30 cts/s. COS ACQ: ------- Variability, from Grankin et al. (2007): 27 U-band observations U=14.02 +/- 0.15 (1-sigma) Umin: 13.73, Umax=14.41 Worst-case scenario: multiply broadband emission by 1.9 MIRRORA: 16 cts/s This is calculated from the HD98800 IUE spectrum. The two spectra match up very well from 3200-5000 A, with HBC 427 being 15 times fainter than HD98800. The HBC 427 observation occurred when U=14.3 (rough estimate), so close to its faintest level. That makes the "worst-case" count rate 30 cts/s. G130M: ------ C II flux: 5.0e-15 erg/cm2/s => 0.0025 cts/s Ly-alpha flux: 1.5e-15 erg/cm2/s (tentative detection) G130M: ------ C II flux: 5.0e-15 erg/cm2/s => 0.0025 cts/s Ly-alpha flux: 1.5e-15 erg/cm2/s (tentative detection) G130M: ------ C II flux: 5.0e-15 erg/cm2/s => 0.0025 cts/s Ly-alpha flux: 1.5e-15 erg/cm2/s (tentative detection) G130M: ------ C II flux: 5.0e-15 erg/cm2/s => 0.0025 cts/s Ly-alpha flux: 1.5e-15 erg/cm2/s (tentative detection) G160M: -------- C IV flux: 1.2e-14 erg/cm2/s => 0.003 cts/s G160M: -------- C IV flux: 1.2e-14 erg/cm2/s => 0.003 cts/s G160M: -------- C IV flux: 1.2e-14 erg/cm2/s => 0.003 cts/s V=11.6 => saturation in 1.6s The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1301463851000 74.74853082777369 (Tic-Visit :proposal-id 11616 :visit-id "27" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:27:51.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1159472 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "27" :obset-id "27" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "27" :obset-id "A7" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "27" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2951 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "27" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3044 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "27" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2934 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) false 3 3 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1301521421000 80.30700473974463 (Tic-Visit :proposal-id 11616 :visit-id "28" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:21.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1159424 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "28" :obset-id "28" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "28" :obset-id "B8" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "28" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2941 :al-overhead-at-end 0 :internal-dur-at-end 107 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "28" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3053 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "28" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2942 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) false 3 0 IUE spectrum: http://www.astro.caltech.edu/~gregoryh/11616/safety/lkca19_iue.dat MIRRORB/PSA: 4.6 cts/s, time for S/N=40 => 50s Variability: Grankin et al. (2008): 61 U-band observations; U=12.54 +/- 0.07 (1-sigma); min-max=0.38 mag i.e., very little variability. Note that this method likely underestimates the amount of variability in the lines, but should be good for the broadband MIRROR images. IUE spectrum: http://www.astro.caltech.edu/~gregoryh/11616/safety/lkca19_iue.dat MIRRORB/PSA: 4.6 cts/s, time for S/N=40 => 50s Variability: Grankin et al. (2008): 61 U-band observations; U=12.54 +/- 0.07 (1-sigma); min-max=0.38 mag i.e., very little variability. Note that this method likely underestimates the amount of variability in the lines, but should be good for the broadband MIRROR images. COS G130M: C II: marginal detection of 1.1e-14 erg/cm2/s => 0.006 cts/s Ly-alpha: Measured Mg II flux (IUE): 1.8e-13 erg/cm2/s estimated Ly-alpha flux: 3.6e-14 erg/cm2/s => 0.022 cts/s in brightest pixel This estimate for Ly-alpha emission does not include the higher N(H I) and extinction to LkCa 19 relative to the nearby cool stars. Variability: Grankin et al. (2008): 61 U-band observations; U=12.54 +/- 0.07 (1-sigma); min-max=0.38 mag i.e., very little variability. Note that this method likely underestimates the amount of variability in the lines, but should be good for the broadband MIRROR images. COS G130M: C II: marginal detection of 1.1e-14 erg/cm2/s => 0.006 cts/s Ly-alpha: Measured Mg II flux (IUE): 1.8e-13 erg/cm2/s estimated Ly-alpha flux: 3.6e-14 erg/cm2/s => 0.022 cts/s in brightest pixel This estimate for Ly-alpha emission does not include the higher N(H I) and extinction to LkCa 19 relative to the nearby cool stars. Variability: Grankin et al. (2008): 61 U-band observations; U=12.54 +/- 0.07 (1-sigma); min-max=0.38 mag i.e., very little variability. Note that this method likely underestimates the amount of variability in the lines, but should be good for the broadband MIRROR images. COS G130M: C II: marginal detection of 1.1e-14 erg/cm2/s => 0.006 cts/s Ly-alpha: Measured Mg II flux (IUE): 1.8e-13 erg/cm2/s estimated Ly-alpha flux: 3.6e-14 erg/cm2/s => 0.022 cts/s in brightest pixel This estimate for Ly-alpha emission does not include the higher N(H I) and extinction to LkCa 19 relative to the nearby cool stars. Variability: Grankin et al. (2008): 61 U-band observations; U=12.54 +/- 0.07 (1-sigma); min-max=0.38 mag i.e., very little variability. Note that this method likely underestimates the amount of variability in the lines, but should be good for the broadband MIRROR images. COS G130M: C II: marginal detection of 1.1e-14 erg/cm2/s => 0.006 cts/s Ly-alpha: Measured Mg II flux (IUE): 1.8e-13 erg/cm2/s estimated Ly-alpha flux: 3.6e-14 erg/cm2/s => 0.022 cts/s in brightest pixel This estimate for Ly-alpha emission does not include the higher N(H I) and extinction to LkCa 19 relative to the nearby cool stars. Variability: Grankin et al. (2008): 61 U-band observations; U=12.54 +/- 0.07 (1-sigma); min-max=0.38 mag i.e., very little variability. Note that this method likely underestimates the amount of variability in the lines, but should be good for the broadband MIRROR images. Measured C IV flux: 2.0e-14 erg/cm2/s => 0.005 cts/s in G160M Measured C IV flux: 2.0e-14 erg/cm2/s => 0.005 cts/s in G160M Measured C IV flux: 2.0e-14 erg/cm2/s => 0.005 cts/s in G160M STIS acquisition: F28x150LP filter: 0.005s for S/N=40; saturation in 0.95s Brightest pixel: 2.7 cts/s @ Mg II for a line with 1.2e-14 erg/cm2/s and FWHM=0.4 A The 0.9e-14 is calculated from the Mg II flux, dividing by 1.5 because the line is a doublet (one is stronger). The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1260168008000 288.3421551223329 (Tic-Visit :proposal-id 11616 :visit-id "29" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:26.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 985472 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "29" :obset-id "29" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "29" :obset-id "C9" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "29" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2986 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "29" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3080 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "29" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2950 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) false 3 3 The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1304571500000 88.16791700283272 (Tic-Visit :proposal-id 11616 :visit-id "30" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:33.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1194224 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "30" :obset-id "30" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "30" :obset-id "B0" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "30" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2968 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "30" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3059 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "30" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2950 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3275 :pcs-gap 0 ) false 3 3 Timing link suitability includes constraints ([Sequence (31 33) within 0.5 days]) The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1283088225000 260.8029210935189 (Tic-Visit :proposal-id 11616 :visit-id "31" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:37.0" :trans-errors '(:WARNINGS 4 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 591648 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "31" :obset-id "31" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "31" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2943 :al-overhead-at-end 0 :internal-dur-at-end 78 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "31" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3036 :al-overhead-at-end 0 :internal-dur-at-end 69 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "31" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 116 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "31" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 428 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 4 4 COS ACQ: -------- Divide gmaur_g230l.dat by 75: 2.2 cts/s in brightest pixel, PSA/MIRRORA COS ACQ: -------- Divide gmaur_g230l.dat by 75: 2.2 cts/s in brightest pixel, PSA/MIRRORA G160M: ------ C IV flux: 1.2e-15 erg/cm2/s => 0.0002 cts/s in brightest pixel G160M: ------ C IV flux: 1.2e-15 erg/cm2/s => 0.0002 cts/s in brightest pixel G160M: ------ C IV flux: 1.2e-15 erg/cm2/s => 0.0002 cts/s in brightest pixel G130M: ------ C II flux: not detected Estimated Ly-alpha flux: 3.8e-15 => 5e-4 cts/s in brightest pixel G130M: ------ C II flux: not detected Estimated Ly-alpha flux: 3.8e-15 => 5e-4 cts/s in brightest pixel G130M: ------ C II flux: not detected Estimated Ly-alpha flux: 3.8e-15 => 5e-4 cts/s in brightest pixel G130M: ------ C II flux: not detected Estimated Ly-alpha flux: 3.8e-15 => 5e-4 cts/s in brightest pixel The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1264140898000 355.2380595896494 (Tic-Visit :proposal-id 11616 :visit-id "32" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:44.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 950720 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "32" :obset-id "32" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "32" :obset-id "C2" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "32" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3343 :al-overhead-at-end 0 :internal-dur-at-end 50 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "32" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3434 :al-overhead-at-end 0 :internal-dur-at-end 362 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "32" :orbit-number 3 :pcs-time 333 :si-vis-utilization 3325 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3633 :pcs-gap 0 ) false 3 3 Timing link suitability includes constraints ([Sequence (31 33) within 0.5 days]) The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1283111254000 258.9920086356715 (Tic-Visit :proposal-id 11616 :visit-id "33" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:47.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 350336 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "33" :obset-id "33" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "33" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2925 :al-overhead-at-end 0 :internal-dur-at-end 324 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "33" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3036 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 2 2 STIS ACQ: saturation in 15-35s Timing link suitability includes constraints ([34 After 13 by 0.1 to 0.1 days]) The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. 1292169767000 46.32777671333861 (Tic-Visit :proposal-id 11616 :visit-id "34" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 472112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "34" :obset-id "34" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "34" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 1 0 V-band mag ranges from 11-12.5 (Grankin et al. 2007). With the [O III] filter and Kurucz K4 SpT, S/N=40 is reached in 2.3-10s This is a copy of failed visit 13 (Tic-Visit :proposal-id 11616 :visit-id "13" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:21:06.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 756880 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "13" :obset-id "13" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "13" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "13" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3025 :al-overhead-at-end 0 :internal-dur-at-end 400 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 2 0 Variability: range of 10 in 5 IUE spectra. Grankin et al. (2007): 94 U-band spectra, U=13.02 +/- 0.72; full range of 12.2-15.2. NUV spectrum: uxtau_lp06978.dat UX Tau: brightest IUE observation is lp06978. S/N is poor at short wavelengths, so lkca15_g230l.dat was used as a template. lkca15_g230l x 4 for the ETC. This IUE spectrum was obtained when U was about 13.3, so variability could increase the count rate by about a factor of 3. MIRRORB: brightest pixel=4.8 cts/s for the brightest IUE spectrum. Multiplying by 3 yields a count rate of 15 cts/s, well below the 50 cts/s limit. Variability: range of 10 in 5 IUE spectra. Grankin et al. (2007): 94 U-band spectra, U=13.02 +/- 0.72; full range of 12.2-15.2. NUV spectrum: uxtau_lp06978.dat UX Tau: brightest IUE observation is lp06978. S/N is poor at short wavelengths, so lkca15_g230l.dat was used as a template. lkca15_g230l x 4 for the ETC. This IUE spectrum was obtained when U was about 13.3, so variability could increase the count rate by about a factor of 3. MIRRORB: brightest pixel=4.8 cts/s for the brightest IUE spectrum. Multiplying by 3 yields a count rate of 15 cts/s, well below the 50 cts/s limit. FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G130M: brightest line is C II 1335, flux=2.3e-14 erg/cm2/s. Using TW Hya as a template yields a count rate of 0.01 cts/s, far below brightness limit. Ly-alpha: based on H-alpha emission, we would expect a Ly-alpha flux of 2.4e-13 erg/cm2/s, if its detected (unlikely), for a maximum count rate of 0.032 cts/s, far below the limit of 0.7 cts/s FUV spectrum: uxtau_iue.dat G160M: brightest line is C IV, flux=9.4e-14 erg/cm2/s. Using TW Hya as a template, brightest pixel is 0.016 cts/s FUV spectrum: uxtau_iue.dat G160M: brightest line is C IV, flux=9.4e-14 erg/cm2/s. Using TW Hya as a template, brightest pixel is 0.016 cts/s FUV spectrum: uxtau_iue.dat G160M: brightest line is C IV, flux=9.4e-14 erg/cm2/s. Using TW Hya as a template, brightest pixel is 0.016 cts/s This is a copy of failed visit 34. (Tic-Visit :proposal-id 11616 :visit-id "34" :proposal-version -1 :trans-version "20100505" :date "31-Oct-2010 20:31:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 472112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "34" :obset-id "34" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "34" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2916 :al-overhead-at-end 0 :internal-dur-at-end 587 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3249 :pcs-gap 0 ) false 1 0 V-band mag ranges from 11-12.5 (Grankin et al. 2007). With the [O III] filter and Kurucz K4 SpT, S/N=40 is reached in 2.3-10s /private/var/folders/z4/z44ymUiuH2iEzitfiilJ1E+++TI/-Tmp-/OPVisit8689926849814699316.xml 1314426219632 This is a copy of failed visit 19. (Tic-Visit :proposal-id 11616 :visit-id "59" :proposal-version -1 :trans-version "20110811" :date "27-Aug-2011 08:23:39.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 985472 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11616 :visit-id "59" :obset-id "59" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 11616 :visit-id "59" :obset-id "A9" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11616 :visit-id "59" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2986 :al-overhead-at-end 0 :internal-dur-at-end 59 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "59" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3088 :al-overhead-at-end 0 :internal-dur-at-end 409 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11616 :visit-id "59" :orbit-number 3 :pcs-time 333 :si-vis-utilization 2968 :al-overhead-at-end 0 :internal-dur-at-end 689 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) true 3 2 STIS.ta.233716 8s = S/N=165, saturation in 94s user: sz102_lris.dat http://etc.stsci.edu/etc/results/STIS.sp.233723/ used: sz102_lris.dat S/N=12s at 3600 , time to saturation = 3600 s (at H-beta) brightest pixel: 9.3 cts/s global count rate (source): 1577 cts/s BOT: --- two objects were flagged by GSC2: (1) 16:08:29.7 -39:03:10.65 (2) 16:08:28.7 -39:03:06.16 Both objects are deemed safe by the BOT. Object (1) is the science target discussed below, Object (2) is very faint. =============================== http://etc.stsci.edu/etc/results/STIS.sp.234647/ =============================== Ca II H: 2.8e-14 erg/cm2/s in Keck/LRIS spectrum TW Hya Ca II H: 2.3e-12 erg/cm2/s in HST G430L Mg II h: 2.1e-12 erg/cm2/s in HST E230M Predicted Mg II h flux: 80 times weaker than TW Hya TW Hya input spectrum with G230L: 2.2 cts/s at 2800 A, much lower than brightness limit of 75 Detector count rate of 4060 cts/s (58 from the spectrum), much lower than limit of 200,000 =============================== http://etc.stsci.edu/etc/results/STIS.sp.234657/ =============================== E230M spectrum o8nz44010_x1d.fits, good for Mg II only: Mg II h: 4.1e-14 erg/cm2/s Maximum count rate: 1.2 cts/s, lower than above because of the weak continuum emission =============================== http://etc.stsci.edu/etc/results/STIS.sp.234659/ =============================== use detau_iue.dat from http://archive.stsci.edu/prepds/iuepms/datalist.html divided by 20 to match optical spectrum of Sz 102 Brightest pixel: 0.22 cts/s Total count rate: 3680 cts/s