0Assigned ID: 548
----- Attempting Submission 1 (Fri Apr 11 16:02:48 GMT 2014) -----
HST Phase I Proposal 548 (Pairs_proposal.apt.2014_04_11_05_12.apt) successfully submitted.
----- Attempting Submission 2 (Fri Apr 11 17:42:50 GMT 2014) -----
HST Phase I Proposal 548 (Pairs_proposal.apt.2014_04_11_05_12.apt.2014_04_11_16_03.aptbackup) successfully submitted.
----- Attempting Submission 3 (Fri Apr 11 20:52:39 GMT 2014) -----
HST Phase I Proposal 548 (Pairs_proposal.apt.2014_04_11_05_12.apt.2014_04_11_16_03.aptbackup.2014_04_11_18_05.aptbackup) successfully submitted.
----- Attempting Submission 4 (Fri Apr 11 21:24:15 GMT 2014) -----Minor changes were made in the proposal description section.1318796933----- Attempting Submission 1 (Tue Jul 22 20:43:25 GMT 2014) -----
HST Phase II Proposal 13852 (Pairs_phaseII.apt) successfully submitted.
----- Attempting Submission 2 (Wed Jul 23 15:35:02 GMT 2014) -----
HST Phase II Proposal 13852 (Pairs_phaseII.apt) successfully submitted.
----- Attempting Submission 3 (Thu Jul 24 15:29:28 GMT 2014) -----How Galaxy Mergers Affect Their Environment: Mapping the Multiphase Circumgalactic Medium of Close Kinematic PairsGalaxy mergers are an important route through which galaxy transformations take place. The interplay of gas between the merging galaxies and their circumgalactic medium (CGM) likely plays a crucial part in this process. Despite its importance, no systematic study has been carried out to study the physical properties of this CGM gas and how it is affected by the merger process. We propose a carefully controlled absorption-line experiment to study the CGM around spectroscopically-identified close kinematic pairs. We plan to obtain COS observations of the CGM around a sample of 11 close kinematic pairs using 8 new QSO sight lines and three archival ones, all within 150 kpc of the interacting galaxy pairs. We will probe the multiphase CGM, using the C IV line to probe the warm gas and H I and other lower ionization metal species, C II Si II/III, to probe the cooler, more dense gas. We will combine these new observations with the complementary COS-Halos and COS-Dwarfs programs, which primarily probe the CGM around isolated galaxies. Using the isolated galaxies as a control sample will allow us to study the effects of the merging process on the CGM gas. Moreover, armed with spectroscopic and morphological information on the kinematic pairs, we will investigate how merger activities such as tidal interactions, affect the CGM of these galaxies. SDSS and COS provide the only means of probing the CGM of a controlled sample of mergers in the local Universe.Our strategic goal is to build a sample of QSO/interacting galaxy pairs with rho < 150 kpc to study multi-phase gas in galactic halos and its dependence on galaxy properties. Together, G130M and G160M range over 1150 - 1750 A, which gives us access to a host of important ionization, density, and metallicity diagnostics, most importantly the C IV doublet, 1548/1550 A, which is a sensitive tracer of highly ionized gas. The galaxy redshifts range from z ~ 0.006 - 0.07, where these ions will be covered on at least one of the grating settings.
Exposure times: Most of our target QSOs are newly discovered by SDSS, and so have not been observed spectroscopically in the UV before. To ensure sufficient flux in the G130M/G160M bands we have cross-referenced our QSO catalog with the GALEX DR4 all-sky survey (AIS) and selected only QSOs with a significant detection in the GALEX FUV band (~ 1500 \AA). Measured GALEX FUV magnitudes for our sample range from 16.10 to 18.60. The redshifts range from z = 0.24 - 1.0. Note that if we assume the FOS composite QSO in the ETC, QSOs in this range of redshift and magnitude are always well below the bright limits of COS for both FUV spectroscopic exposures and NUV imaging target acquisitions with MIRRORB (and MIRRORA for two targets).
We use the COS online ETC to calculate that we will achieve S/N = 8-12 per resolution element over 1150 - 1750 A with 2-7 orbit exposures for our target objects. The exposure time is roughly equally divided between the two gratings. Use of the GALEX fluxes means that we do not need to correct for interstellar extinction, which in any case is E(B-V) <~ 0.1 for these high-latitude targets. Each visit has one central wavelength per grating packed for maximim efficiency, with the central wavelengths chosen to detect the absorption lines of interest. Based on our experience with the ETC for QSOs in this range of redshift and magnitude and with our ~90 similar objects observed in Cycle 17-18, we know that these spectra always have their brightest pixel at the position of geocoronal Lyman alpha emission, not from the QSO source. These objects never get close to the bright limits, whatever the magnitude, redshift, or central wavelength setting.
Notes on Acquisitions:
Our coordinates are all from SDSS, with astrometry good to 100 mas, so we adopt NUV imaging (ACQ/IMAGE) for all targets. Our experience in Cycle 17/18 is that IMAGE acqisitions are working well for these targets. We compute the exposure times for each target using the COS Imaging Target acquisition ETC. We use MIRRORB for all cases except VV2006-J101541.1+594445 and VV2006-J222836.3-095009, where the targets are faint enough to use MIRRORA for acquisition (ETC COS.ta.623560), (ETC COS.ta.625115).
As anticipated for these targets selected from SDSS+GALEX, the BOT returns no health-and-safety issues for the targets or their fields.
We divide our visits to 2, 3 and 4 orbit visits respectively. Three targets with 6 and 7 orbits of observations are divided into two visits with (3+3 orbits) and (3+4 orbits) respectively. The Targets and their orbits are tabulated below.
------------------------
ICRF-J122011.8+020342 (2-orbit, Visit 01)
cenwave 1291 for G130M
cenwave 1600 for G160M
------------------------
VV2006-J140658.8+144238 (2-orbit, Visit 02)
cenwave 1291 for G130M
cenwave 1611 for G160M
------------------------
QSO-B0952+457 (3-orbit, Visit 03)
cenwave 1291 for G130M
cenwave 1600 for G160M
------------------------
QSO-B01139+305 (3-orbit, Visit 04)
cenwave1589 for G160M
------------------------
VV2006-J092542.3+344108 (4-orbit, Visit 05)
cenwave 1291 for G130M
cenwave 1611 for G160M
------------------------
VV2006-J115412.1+463552 (First visit =3 orbit out of 6, Visit 06)
cenwave 1300 for G130M
------------------------
VV2006-J115412.1+463552 (Second visit =3 orbit out of 6, Visit 07)
cenwave 1600 for G160M
------------------------
VV2006-J222836.3-095009 (First visit =3 orbit out of 7, Visit 08)
cenwave 1291 for G130M
------------------------
VV2006-J222836.3-095009 (Second visit =4 orbit out of 7, Visit 09)
cenwave 1611 for G160M
------------------------
VV2006-J101541.1+594445 (First visit =3 orbit out of 7, Visit 10)
cenwave 1291 for G130M
------------------------
VV2006-J101541.1+594445 (Second visit =4 orbit out of 7, Visit 11)
cenwave 1611 for G160M
------------------------
The central wavelengths are set to optimally cover the interesting absorption lines from the galaxies of interest (mainly Lya and C IV). Thus almost every cenwave setting allowed for COS used for one target or another. The representative ETCs show that geocoronal Lya is always the brightest spot in G130M regardless of the cenwave, but is still well below the limits (0.1 cts at Lya vs. 0.67 cts limit), and the targets tend to be at least an order of magnitude fainter. Since the FOS template spectrum is relatively flat (see the representative cases) the global count rate is almost invariant with cenwave and never gets close to the limits.QUASAR ABSORPTION LINES AND IGMDefaultfalsetruefalsefalsefalseSUPPORTEDGALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=17.85GALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=17.45GALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.6GALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.36GALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV= 18.47GALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=16.10GALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000FUV=16.77GALAXYQSOQUASARThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000FUV=18.6COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1611COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG130M1300COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/FUVSpectroscopicNoNoG160M1611The scheduling data was generated by CASM 22.2.CASM was run in Phase II mode./Users/bordoloi/Dropbox/COS-Pairs/PhaseII/OP-cache/Pairs_phaseII-v01.xml2-orbit Visit
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