0 Assigned ID: 362 ----- Attempting Submission 1 (Fri Mar 06 00:47:37 GMT 2020) ----- HST Phase I Proposal 362 successfully submitted. Receipt: # 362-1 ----- Attempting Submission 2 (Fri Mar 06 06:18:45 GMT 2020) ----- If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. If the target position is not known to 0.4" (or better), an ACQ/SEARCH should precede the ACQ/IMAGE. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. This resubmission corrects the FP-POS pattern for Visit 7 of the program, changing FP-POS=4 which was set for 5 of the 6 sub-exposures, to an alternating pattern of FP-POS=3 and FP-POS=4 for the sub-exposures. -15010624 ----- Attempting Submission 1 (Mon Jun 22 06:19:58 GMT 2020) ----- ----- Attempting Submission 2 (Wed Jun 16 22:46:39 GMT 2021) ----- Impossible to implement a full set of FP-POS as there are only 2 for the 1291 setting of the G130M. For the two FP-POS settings, FP-POS=3 is always selected first before FP-POS=4; this follows the "most effecient order" as stated in the IHB of 1, 2, 3 & 4 when 1 & 2 doesn't exist. Objects 1-3 have positions estimated from previous HST data, and are accurate to < 0.3 arcsec; their ACS therefore need only ACQ/IMAGE. We propose a COS G130M program to measure the gas-phase metallicities of the cool neutral medium in 5 "extremely metal poor galaxies", or XMPGs. We have selected the XMPGs to have emission line metallicities, Z_emm, in the range 12+log(O/H) = 7.1 to 7.5, or 1/40th to 1/16 times the solar metallicity. The COS spectra of the UV-bright regions in the galaxies will record, in particular, Lyman-alpha, SII, PII, NI, CII and OI absorption lines, which can be used to derive accurate column densities and therefore abundances and abundance ratios. We aim to test how much less the metallicity of the neutral medium, Z_abs, can be, compared to Z_emm, a difference that is seen in higher metallicity star-forming galaxies. We also aim to provide accurate N/O and alpha/O abundance ratios in the XMPGs' neutral gas from which to investigate their star formation histories. Two unique galaxies are targeted, DDO 68, which is one of the lowest metallicity galaxies known, and SBS 0940+544, a galaxy where Z_emm drops by a dex over a transverse length of only 400 pc. Confirming differences in Z_abs and Z_emm in XMPGs will show that the baseline metallicity for the canonical stellar-mass to metallicity relationship should use Z_abs instead of Z_emm in galaxy evolution modelling. We will also use our data to explore whether XMPGs could be the progenitors of young galaxies seen by the damped Lyman-alpha absorption systems detected towards background QSOs, or whether the origin of the latter population still needs to be properly explained. Our aim is to observe the brightest regions of the selected XMPGs with the COS G130M grating to record Lyman-alpha absorption and metal absorption lines from the interstellar gas in and around the galaxy. The galaxies range in redshift from ~ 500 - 3600 km/s, so, e.g., Lyman-alpha lies between 1218-1230A. 3 of 5 sightlines have been observed by COS before, either at lower resolution with the G140L grating, or at longer wavelengths (e.g. with the G185M grating), so information already exists on UV fluxes and previous ACQ exposure times. These are discussed in this Phase 2 for each object individually. UV fluxes for the remaining 2 sightlines are extrapolated from optical SDSS spectra. For all sightlines, we use the 2 FP-POS settings allowed for the grating centered at 1291A, a wavelength which is essential for observing the Lyman-alpha absorption. For one sightline (DDO68-1), one of the 2 visits needs to be spent in SHADOW, in order to resolve the Lyman-alpha absorption line profile from strong geocoronal Lyman-alpha emission. Dr. David Bowen is a Research Astronomer in the Astrophysical Sciences department of Princeton University. He has over 30 years experience designing experiments to study the distribution of baryons in the universe. He has lead more than 24 programs using HST, the Far Ultraviolet Spectroscopic Explorer (FUSE) and the Galaxy Evolution Explorer (GALEX). Prof. Todd Tripp is a professor at the Univ. of Mass and is one of the preeminent experts in the study of the intergalactic medium and the circumgalactic medium (CGM), as well as the ISM of our own Milky Way. He too has extensive expertise in the analysis of HST data and has led several large COS programs. Prof. Max Pettini is a professor at the Institute of Cambridge in the UK; he has lead the field in the interpretation of abundances at both low and high redshift for many decades. Galaxies Intergalactic Medium and the Circumgalactic Medium 6 false false true false false false false SUPPORTED EXT-CLUSTER STAR FORMING REGION YES The position of the star-forming region is based on the previous COS observations (P13788) and agrees with (a) its position on the WFC3 UVIS F275W image retrieved from the Hubble Legacy Archive, and (b) its position on the 22 sec MIRROR-B ACQ/IMAGE exposure used to acquire the object in P13788 (lcne01qzq_flt.fits). UGC5340 J2000 J2000 FUV(1460) flux = 1.0e-15 ergs/cm^2/s/A (based on previous COS G160M data) EXT-CLUSTER STAR FORMING REGION YES The position of the star-forming region is measured from a 160sec COS MIRROR-A ACQ image (ldaf03pxq_flt.fits) taken as part of P14628 for a COS G140L observation. Image shows several point sources all confined to a radius ~ 0.3 arcsec, but assume EXTENDED. SDSJ120202.49+541551.05 J2000 J2000 F(1220) = 1.3e-15 ergs/cm^2/s/A EXT-CLUSTER STAR FORMING REGION NO Position of star cluster is measured from a 9 sec COS ACQ MIRROR-A image (ldkm04zbq_flt.fits) obtained as part of G140L observations (P15220) SDSSJ094416.59+541134.3 J2000 J2000 F(1220) = 1.4e-15 ergs/cm^2/s/A EXT-CLUSTER STAR FORMING REGION YES Co-ords are taken from the brightest central point seen in SDSS. No HST data exists in the Archive to better verify fluxes or position. SDSSJ012646.39-003845.6 J2000 J2000 F(1220) = 1.5e-15 ergs/cm^2/s/A EXT-CLUSTER STAR FORMING REGION YES Flux calculated from SDSS spectrum and assuminf a power-law SED with alpha = -1.5. No HST data exists in the Archive to better verify fluxes or position. J2000 J2000 F(1220) = 1.3e-15 ergs/cm^2/s/A COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1291 1592806609996 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. We require that the visit is spent in SHADOW, in order to minimize the effects of geocoronal Lyman-alpha emission. 1613831305000 163.0 (Tic-Visit :proposal-id 16227 :visit-id "01" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:16:49.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 122016 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "01" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2137 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset 316 :dark-utilization 1821 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 1899 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset 0 :dark-utilization 1899 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 1899 :al-overhead-at-end 0 :internal-dur-at-end 341 :dark-offset 0 :dark-utilization 1899 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) true 3 0 Examination of a 22 second COS ACQ image taken as part of the P13788 G160M observations (lcne01qzq_flt.fits) shows that 22 seconds with MIRROR-B gives ~ 20 counts in a 9x9 pix^2 (0.23x0.23 arcsec^2) box, which is inadequate for a reliable ACQ. The count-rate recorded is equivalent to F(1580) ~ 2e-16 cgs for a power-law SED that varies as lambda^-3.5. [This exponent is estimated from fluxes at 1460A (G160M), 1740A (G185M), 2750A (MAG_AUTO estimates from the WFC3 F275W HLA data), and 3600A (ground based spectrophometry published by Annabali et al 2019 (MNRAS, 482, 3892).] (NB. This flux is ~ one-quarter that measured through the full 2.5" aperture and G160M grating.) Switching to MIRROR-A, to reach a S/N of 20, we require a 35 sec exposure. 1592806090225 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1604520133000 293.0656469660644 (Tic-Visit :proposal-id 16227 :visit-id "02" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:09.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 165456 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "02" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2771 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "02" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2772 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "02" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2772 :al-overhead-at-end 0 :internal-dur-at-end 350 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3165 :pcs-gap 0 ) true 3 0 Examination of a 22 second COS ACQ image taken as part of the P13788 G160M observations (lcne01qzq_flt.fits) shows that 22 seconds with MIRROR-B gives ~ 20 counts in a 9x9 pix^2 (0.23x0.23 arcsec^2) box, which is inadequate for a reliable ACQ. The count-rate recorded is equivalent to F(1580) ~ 2e-16 cgs for a power-law SED that varies as lambda^-3.5. [This exponent is estimated from fluxes at 1460A (G160M), 1740A (G185M), 2750A (MAG_AUTO estimates from the WFC3 F275W HLA data), and 3600A (ground based spectrophometry published by Annabali et al 2019 (MNRAS, 482, 3892).] (NB. This flux is ~ one-quarter that measured through the full 2.5" aperture and G160M grating.) Switching to MIRROR-A, to reach a S/N of 20, we require a 35 sec exposure. 1592806092100 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1619859033000 143.60000000000002 (Tic-Visit :proposal-id 16227 :visit-id "03" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:11.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 208960 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "03" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2936 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "03" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2938 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "03" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2938 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) true 3 0 Exposure time is based on the flux measured from previous COS G140L observations [P14628, F(1220)=1.3e-15 cgs] and assuming that the SED follows a power law that varies as lambda^(-2.5). Exposure time is set to give a S/N of 20. A previous 160 sec COS ACQ image (ldaf03pxq_flt.fits) for the same G140L observations shows that this exposure time gives a good S/N (e.g. 1600 counts from source+bg in a 0.23x0.23 arcsec box centered on the brightest spot in the image). 1592806093886 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1619950484000 143.60000000000002 (Tic-Visit :proposal-id 16227 :visit-id "04" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:13.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 208960 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "04" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2936 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "04" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2938 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "04" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2938 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) true 3 0 Exposure time is based on the flux measured from previous COS G140L observations [P14628, F(1220)=1.3e-15 cgs] and assuming that the SED follows a power law that varies as lambda^(-2.5). Exposure time is set to give a S/N of 20. A previous 160 sec COS ACQ image (ldaf03pxq_flt.fits) for the same G140L observations shows that this exposure time gives a good S/N (e.g. 1600 counts from source+bg in a 0.23x0.23 arcsec box centered on the brightest spot in the image). 1592806095327 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1602877234000 303.6628397138131 (Tic-Visit :proposal-id 16227 :visit-id "05" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:14.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 174144 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "05" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2940 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "05" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2940 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "05" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2940 :al-overhead-at-end 0 :internal-dur-at-end 350 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) true 3 0 From a previous 9 sec COS ACQ IMAGE with MIRROR-A (P15220, ldkm04zbq_flt.fits) the count-rate (source+bg) within a 0.23x0.23 box centered on the star cluster is 18 counts/sec. So a 23 sec exposure should give a S/N ~ 20 in the same box. 1592806096727 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1615626431000 146.449519910376 (Tic-Visit :proposal-id 16227 :visit-id "06" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:16.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 174144 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "06" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2940 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "06" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2940 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "06" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2940 :al-overhead-at-end 0 :internal-dur-at-end 350 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) true 3 0 From a previous 9 sec COS ACQ IMAGE with MIRROR-A (P15220, ldkm04zbq_flt.fits) the count-rate (source+bg) within a 0.23x0.23 box centered on the star cluster is 18 counts/sec. So a 23 sec exposure should give a S/N ~ 20 in the same box. 1623883411553 /private/var/folders/3w/3cmkcm694574ksd8zvyxvkgh0000gn/T/OPVisit17713924107988164784.xml The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16227 :visit-id "07" :proposal-version -1 :trans-version "20200619" :date "16-Jun-2021 18:43:31.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 295888 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "07" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2739 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "07" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "07" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2749 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 No HST data exists for this object. F(4000) = 4e-16 cgs from SDSS spectrum of central region, and suggests a power-law SED that varies as lambda^(-1.8). 1592806100103 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1611381280000 70.17711868982971 (Tic-Visit :proposal-id 16227 :visit-id "08" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:19.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 295888 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "08" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2739 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "08" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "08" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2750 :al-overhead-at-end 0 :internal-dur-at-end 379 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 No HST data exists for this object. F(4000) = 4e-16 cgs from SDSS spectrum of central region, and suggests a power-law SED that varies as lambda^(-1.8). 1592806102034 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1604857562000 293.3001340742217 (Tic-Visit :proposal-id 16227 :visit-id "09" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:21.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 261136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "09" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2743 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "09" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2747 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "09" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2747 :al-overhead-at-end 0 :internal-dur-at-end 369 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 Assuming (F4000) = 5e-16 and alpha=-1.5 from SDSS spectrum of the central source. S/N of 68 for this exposure time (4600 counts in brightest pix) 1592806103447 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1604777485000 293.3001340742217 (Tic-Visit :proposal-id 16227 :visit-id "10" :proposal-version -1 :trans-version "20200518" :date "22-Jun-2020 02:08:23.0" :trans-errors '(:WARNINGS 2 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 261136 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16227 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16227 :visit-id "10" :orbit-number 1 :pcs-time 393 :si-vis-utilization 2743 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "10" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2747 :al-overhead-at-end 0 :internal-dur-at-end 76 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16227 :visit-id "10" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2747 :al-overhead-at-end 0 :internal-dur-at-end 369 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3142 :pcs-gap 0 ) true 3 0 Assuming (F4000) = 5e-16 and alpha=-1.5 from SDSS spectrum of the central source.