0 Assigned ID: 168 ----- Attempting Submission 1 (Wed Apr 06 21:01:32 GMT 2016) ----- If the target coordinates are 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. 0 ----- Attempting Submission 1 (Wed Jul 13 09:04:05 GMT 2016) ----- One warning refers to the use of ACQ/IMAGE. We have a very good WCS solution from 2MASS stars in HST imaging data, and used an idetical procedure to successfully acquire the same target in GO 13656. The target acquisition used here is a copy of that program. Four warnings refer to the fact we are doing spectroscopy of diffuse emission with the PSA under LP3. This is a minor effect, and our team has a great deal of experience and substantial custom machinery for reducing COS spectra. Recent Cycle 22 observations, with both ACS and COS, have revealed a halo of OVI emission surrounding a low-redshift, compact star-forming galaxy. This is the first time that the coronal gas phase, with the illusive temperature of T~300,000 K, has been mapped in emission for an individual galaxy. The implications of this are profound, in that this gas may represent the hitherto unobservable temperature regime through which galaxy superwinds can radiate energy. These unique observations enable us measure a large number of properties of the warm outflow, but the global properties of the wind in all other gas phases remain illusive because few suitable metal lines are available in the existing COS/G130M spectrum. We propose to obtain COS spectroscopy in the redder G160M setting to measure the absorption features of 10 more interstellar lines. From this we will build a picture of the velocity structure of the outflow in the colder atomic phases that are likely to contain the bulk of the mass. This will provide the complete energetic picture of the outflow, including warm/coronal and colder/atomic phases for the first time. A further G130M spectrum positioned in the halo will determine the properties (flux and kinematics) of a peculiar 'blob' of enhanced OVI emission. This region is as bright in OVI as the central pointing, but is located 10 optical scale lengths from the center, with no obvious cospatial source of excitation. Kinematics derived from this observation will determine its physical origin. This programme will obtain spectra with COS of a single galaxy that hosts an extreme starburst. The object has a very luminous compact central object, with a diffuse gaseous halo. We will obtain: A. COS/G160M spectroscopy on the central pointing (2 orbits) B. G130M spectroscopy in the halo, offset by {ra,dec} = {-1.86,2.13} arcsec (2 orbits) The four orbit allocation will be executed in one visit. We will use the PSA, ACQ/IMAGE, and MIRROR A. The acquisition is a copy of that used in GO 13656, which obtained COS specroscopy (G130M) on the central poiting. After this initial acquisition we will obtain the G160M spectrum of the central pointing (part A. above) We will then perform an offset to a pointing in the halo, re-image the galaxy in the NUV, change grating to G130M, and execute part B. Acquisition time is 13 seconds for SNR=40 assuming a point-source. In part A we use G160M, CENWAVE=1600, TIME-TAG, and all FP positions In part B we use G130M, CENWAVE=1318, TIME-TAG, and all FP positions Each individual specturm is roughly half an orbit. Galaxies 12 false true false false false false SUPPORTED GALAXY DWARF COMPACT NUCLEUS STARBURST NO These target data are copied from GO 13656, which successfully observed the galaxy with COS. J2000 J2000 FUV magnitude 18.8 AB GALAXY HALO STAR FORMING REGION YES These target data are offset by {ra,dec} = {-1.86,2.13} arcsec, as measured in HST images. offset in RA = 1.8573139999999967 arcseconds = 1.8573139999999967 / 3600 / cos(50.139494444 / 180 * pi) = 0.00080496788894599393 offset in DEC = 2.1318730000000016 arcsec = 2.1318730000000016 / 3600 = 0.0005921869444444448 degrees. RA halo = 179.12762708333332 - 0.00080496788894599393 = 179.12682211544438 degrees DEC halo = 50.139494444444445 + 0.0005921869444444448 = 50.140086631388 This is 11:56:30.4373, 50:08:24.31, as entered. J2000 J2000 FUV magnitude 18.8 AB COS/FUV Spectroscopic No No G130M 1318 COS/FUV Spectroscopic No No G160M 1577 1468400117479 /Users/matthew/Dropbox/C24_phaseII/OP-cache/ovi_j1156_spec_c24-v01.xml The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. Photometry that guides target acquisition and integration times is done with HST data from visits 1 and 30 from GO 13656. Flux was measured on the brightest UV source in 0.2 arcsec (acquisition) and 1.25 arcsec (spectroscopic observation) apertures, using the F140LP and F390W filters. Then we interpolated (power-law) between the two, to lambda=2300 AA. Fluxes are quoted in the Comments section of the Acquisition. HST datasets used for the photometry: F140LP : JCME01010 F390W : ICME30010 (Tic-Visit :proposal-id 14601 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "13-Jul-2016 10:55:16.0" :trans-errors '(:WARNINGS 0 :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 165600 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14601 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14601 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3056 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14601 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3169 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14601 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3180 :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 3403 :pcs-gap 0 ) (Tic-Orbit :proposal-id 14601 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3168 :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 3403 :pcs-gap 0 ) true 4 0 F140LP full = 45.660 adu/sec = 1.2387e-15 cgs/AA F140LP ACQ = 27.489 adu/sec = 7.4575e-16 cgs/AA F390W full = 335.631 adu/sec = 1.7145e-16 cgs/AA F390W ACQ = 227.063 adu/sec = 1.1599e-16 cgs/AA COS/NUV full = 6.5052e-16 cgs/AA COS/NUV ACQ = 4.068e-16 cgs/AA These numbers (and the beta slope) were entered into the acquisition and spectroscopic ETCs. There are four observations take, one on each of the FP-POS positions. To estimate the performance we use the COS-aperture flux measured in the F140LP frame. (central wavelength ~1500 AA) F140LP full = 45.660 adu/sec = 1.2387e-15 cgs/AA The exposure time is taken to be 1500 seconds for all integrations. A POS-TARG is executed first. This observation is to obtain a short NUV image to confirm the pointing of the telescope after the POS-TARG. The aim is to detect the NUV continuum at SNR=20. We adopt the following calculation: In ACS/SBC/F140LP flux = 2.5708e-17 cgs/AA In WFC3/UVIS/F390W flux = 1.518e-18 cgs/AA ==> Beta = -0.7998 ==> COS/NUV flux at 2200 AA = 2.0109e-17 cgs/AA For this we aim to detect a single emission line, the flux of which is estimated from the continuum-subtracted OVI image. Line at Center 1283.0 FWHM 0.54 Flux 4.1e-16 The continuum, as estimated in the calculation for Exposure 6, is extremely weak and likely to be undetected in spectroscopic mode. We adopt 1500 seconds as the exposure time, giving SNR=2.97 per exposure. This will then total SNR~6 PER RESEL in the combined spectrum. For this we aim to detect a single emission line, the flux of which is estimated from the continuum-subtracted OVI image. Line at Center 1283.0 FWHM 0.54 Flux 4.1e-16 The continuum, as estimated in the calculation for Exposure 6, is extremely weak and likely to be undetected in spectroscopic mode. We adopt 1500 seconds as the exposure time, giving SNR=2.97 per exposure. This will then total SNR~6 PER RESEL in the combined spectrum. For this we aim to detect a single emission line, the flux of which is estimated from the continuum-subtracted OVI image. Line at Center 1283.0 FWHM 0.54 Flux 4.1e-16 The continuum, as estimated in the calculation for Exposure 6, is extremely weak and likely to be undetected in spectroscopic mode. We adopt 1500 seconds as the exposure time, giving SNR=2.97 per exposure. This will then total SNR~6 PER RESEL in the combined spectrum. For this we aim to detect a single emission line, the flux of which is estimated from the continuum-subtracted OVI image. Line at Center 1283.0 FWHM 0.54 Flux 4.1e-16 The continuum, as estimated in the calculation for Exposure 6, is extremely weak and likely to be undetected in spectroscopic mode. We adopt 1500 seconds as the exposure time, giving SNR=2.97 per exposure. This will then total SNR~6 PER RESEL in the combined spectrum.