0Assigned ID: 799
----- Attempting Submission 1 (Fri Apr 07 19:43:08 GMT 2017) -----For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.
For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.0----- Attempting Submission 1 (Fri Jul 14 18:16:54 GMT 2017) -----
HST Phase II Proposal 15250 (HE0047A.apt) successfully submitted.
Receipt: # 15250-1
----- Attempting Submission 2 (Mon Jul 17 19:06:12 GMT 2017) -----
HST Phase II Proposal 15250 (HE0047A_v2.apt) successfully submitted.
Receipt: # 15250-2
----- Attempting Submission 3 (Tue Jul 18 23:52:03 GMT 2017) -----
----- Attempting Submission 4 (Wed Dec 05 21:11:11 GMT 2018) -----
HST Phase II Proposal 15250 (15250_phase2resubmit.apt) successfully submitted.
Receipt: # 15250-4
----- Attempting Submission 5 (Wed Dec 05 21:11:25 GMT 2018) -----We have allocated multiple FP-POS for each central wavelength settings:
2 FP-POS offsets for C1291 and C1611.
4 FP-POS offsets for C1327, C1589, C1600
Justification for C1291 and C1611:
1)FP-POS=3,4 are the only offset positions available for C1291 cenwave setting, due to the new
COS2025 requirements.
2)For C1611, all 4 FP-POS positions are already used for each of the other three gratings.
Combining 4 different cenwave settings and the different FP-POS leads to an effective
14 different FP-POS offsets for the G160M observations, which should be sufficient to minimize
fixed pattern noise.Resolving the Multiphase ISM of an Elliptical Galaxy at z~0.4Nearly 40% of elliptical galaxies are found to contain cool gas but exhibit no on-going star formation, indicating that some feedback mechanisms are at work. While AGN feedback is commonly thought to be responsible for quenching star formation in massive halos, recent work has reiterated the importance of feedback from old stellar populations, including Type Ia supernovae (SNe Ia). In Zahedy et al. (2016), we reported detections of strong MgII absorption with rest-frame absorption equivalent width of Wr~4 Ang at two locations separated by 8 kpc in projected distance in the ISM of a z=0.408 massive elliptical. The most striking finding is a uniform, super-solar Fe/Mg ratio across a large line-of-sight velocity range of ~700 km/s. The observed super-solar Fe/Mg ratio suggests a large contribution of SNe Ia (>20%) in chemical enrichment. Follow-up low-resolution FUV spectroscopy with HST/STIS allowed us to measure a neutral hydrogen column density of log N(HI)~19.5 and metallicity of ~1/3 solar for both absorbers. Remarkably, the STIS spectra also revealed additional strong absorption features (Wr>1 Ang) that are consistent in wavelength with CII, CIII, NII, NIII, and OVI absorption lines, indicating the presence of a complex, multiphase ISM in this elliptical. Here we propose to use COS with the G130M and G160M gratings to spectrally resolve these low- to high-ionization lines in one absorber. The proposed high-resolution COS spectra will allow us to constrain both the column densities and velocity profiles of individual ions, providing a unique opportunity to resolve the thermal state and ionization condition in the ISM of an intermediate-redshift elliptical galaxy.We will obtain high-resolution (R~17000) FUV spectra of the brighter image of the doubly lensed QSO HE0047-1756, using COS and the G130M and G160M gratings. The primary goal of the proposed FUV spectroscopic observations is to spectrally resolve both low- and high-ionization metal absorption in the ISM of the lensing galaxy, a massive elliptical galaxy at z~0.4.
Exposure Time Estimation:
We aim to reach a signal-to-noise ratio (S/N) level that will allow us to resolve individual components within a strong absorption system. Based on our previous experience with COS data as well as simulated COS spectra, we find that a signal-to-noise ratio of S/N > 10 is sufficient for reaching the goal. From GALEX observations of the HE0047-1756 field, the estimated FUV magnitude of the brighter image of this lensed QSO, HE0047-1756A, is AB(FUV) = 18.7. Using the latest version of the COS exposure time calculator (v25.2) with the FOS QSO spectral template redshifted to z_em = 1.676 and scaled to the FUV magnitude of HE 0047-1756A, we estimate that the total exposure times required to reach the targeted mean S/N ~ 10 are 4 orbits for G130M and 7 orbits for G160M.
Observing Strategy:
The observations will be performed in three separate HST visits, each 3-4 orbits long. COS with the G130M and G160M gratings provide sufficient resolution (FWHM ~ 20 km/s) to resolve the low- and high-ionization absorption lines of this system into distinct kinematic components. For G130M, we will use two central wavelength settings, C1291 (both A and B segments) and C1327 (with the B segment turned off). For G160M, we will use four central wavelength settings, C1577, C1589, C1600, and C1611, in order to reach a uniform S/N over the full spectral range. Furthermore, to reduce the effects of fixed pattern noise in the resulting spectra, we will use multiple FP-POS offsets for each central wavelength setting (two positions for C1291 and C1611, and four positions for the remaining central wavelength settings).
Onboard target acquisition of the QSO will be performed in the first orbit of each visit, by obtaining an NUV image in ACQ/IMAGE mode. Additional ACQ/SEARCH mode acquisition is not necessary, because the coordinates of the target are known to better than 0.25". The estimated GALEX NUV magnitudes of the target QSO image is AB(NUV)=17.8. The Bright Object Tool indicates that MIRROR B is needed in the ACQ/IMAGE mode in order to avoid exceeding the brightness limit. Using the COS Target Acquisition ETC, we find that to obtain a S/N=40 in the acquisition image, a 100s exposure is necessary using MIRROR B. To reduce potential confusion caused by light from the fainter QSO image B (1.4" away from the target), we impose an ORIENT constraints of 125/305 degrees (with an allowed range of +/-45 degrees), in order to maximize the distance between the two QSO images in the cross-dispersion direction.Galaxies and the IGM6falsefalsetruefalsefalsefalsefalseSUPPORTEDEXT-MEDIUMABSORPTION LINE SYSTEM - EXTRAGALACTICBULGEDARK CLOUDHALOHI CLOUDNOJ2000J2000GALEX FUV (AB)=18.7, GALEX NUV(AB) = 17.8COS/FUVSpectroscopicNoNoG130M1327COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1589The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.There are two nearby targets to HE0047A that need to aligned in the cross-dispersion (XD) so that the PSA/MIRRORB target acquisition (TA) will not co-add the light from the multiple targets and MIRRORB spots causing potential confusion during the TA. This XD alignment will also disperse the light from the three targets above or below the prime spectrum. This will allow custom extraction of all sources for cross-contamination analysis.
The targets are approximately aligned along the ORIENT=305/125 angle. We allow a range of +/- 45 degrees, so our Orient requirements are:
260 < ORIENT < 350 OR 80 < ORIENT < 170
There is no requirement for a common alignment between the visits.(Tic-Visit
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)true30The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.There are two nearby targets to HE0047A that need to aligned in the cross-dispersion (XD) so that the PSA/MIRRORB target acquisition (TA) will not co-add the light from the multiple targets and MIRRORB spots causing potential confusion during the TA. This XD alignment will also disperse the light from the three targets above or below the prime spectrum. This will allow custom extraction of all sources for cross-contamination analysis.
The targets are approximately aligned along the ORIENT=305/125 angle. We allow a range of +/- 45 degrees, so our Orient requirements are:
260 < ORIENT < 350 OR 80 < ORIENT < 170
There is no requirement for a common alignment between the visits.154457664900081.76470999999998(Tic-Visit
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)true40The scheduling data was generated by CASM 26.2.2.CASM was run in Phase II mode.There are two nearby targets to HE0047A that need to aligned in the cross-dispersion (XD) so that the PSA/MIRRORB target acquisition (TA) will not co-add the light from the multiple targets and MIRRORB spots causing potential confusion during the TA. This XD alignment will also disperse the light from the three targets above or below the prime spectrum. This will allow custom extraction of all sources for cross-contamination analysis.
The targets are approximately aligned along the ORIENT=305/125 angle. We allow a range of +/- 45 degrees, so our Orient requirements are:
260 < ORIENT < 350 OR 80 < ORIENT < 170
There is no requirement for a common alignment between the visits.(Tic-Visit
:proposal-id 15250
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:date "05-Dec-2018 14:26:50.0"
: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 661056
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)true40