Assigned ID: 672
----- Attempting Submission 1 (Fri Feb 24 20:36:16 GMT 2012) -----
The layout of all 3-orbit visits (visits 05-13) was changed to get about twice the exposure
time in G160M as in G130M. This was achieved by having orbit 1 with the acquisition image
and 2 exposures in G160M (FP-POS=1,2), orbit 2 with 2 exposures in G160M (FP-POS=3,4),
and orbit 3 with 4 exposures in G130M (FP-POS=ALL).
----- Attempting Submission 1 (Tue Jul 10 20:04:39 GMT 2012) -----
----- Attempting Submission 2 (Mon Jul 23 17:26:54 GMT 2012) -----
----- Attempting Submission 3 (Mon Sep 10 19:38:18 GMT 2012) -----
There are warnings about the positional accuracy in the case of ACQ/IMAGE without ACQ/SEARCH. These can be ignored because our positional accuracies are better than 0.4".
UV Spectroscopy of Lyman Break Galaxy Analogs: A Local Window on the Early Universe
UV-selected galaxies at high redshift (LBGs at z~3-10) are the most direct tracers of the early evolution of galaxies and the IGM, but it is difficult to investigate these faint and distant objects in detail. To address this, we have been performing a major program using GALEX and the SDSS to find and study the only type of nearby galaxy that shares many properties with LBGs. These local "Lyman Break Analogs" (LBAs) resemble LBGs in terms of morphology, size, UV luminosity, SFR, mass, velocity dispersion, metallicity, and dust content, allowing us to use them as local laboratories for better understanding of the relevant processes at high-z. Our data includes UV/optical imaging with HST (95 orbits in Cy15-16), X-ray (Chandra, XMM), optical/NIR spectroscopy (VLT, Keck), infrared (Spitzer, Herschel) and radio (VLA, VLBI).
Our Cycle 17 exploratory program with COS revealed numerous new details based on a small sample of LBAs with direct implications for high-z. Most intriguingly, we found strong connections between extreme SN-driven winds (v~1000 km/s), a non-uniform covering by neutral hydrogen, complex Lya profiles, and interstellar absorption lines highly suggestive of a non-zero Lyman continuum escape fraction. Following the tenfold increase in the area surveyed in the UV by GALEX, we have compiled the largest statistical sample of LBAs to date, including many new targets bright enough for COS. We wish to extend our sample size by a factor of 3 to robustly characterize these extraordinary starbursts in the UV. In so-doing it will also shed new light on the complex astrophysics of starbursts, galaxy formation, and enrichment and heating of the IGM in the early universe.
- Each target will be observed with COS/FUV/PSA in grisms G130M and G160M using TIME-TAG mode. Exposures are taken at all FP-POS. We set FLASH=yes for better wavelength calibration.
- For BUFFER-TIME, we assumed a point source flat (in Fnu) with a total FUV magnitude within the COS aperture esimated based on the GALEX flux and the u-band sizes. The buffer time is the shorter value of 2/3 times the buffer time returned by the ETC and the exposure time (was always the exposure time). We further set BUFFER-TIME=EXPOSURE TIME - 100, as recommended by the COS instrument handbook.
- SCHEDULABILITY was set to 100% for all targets.
- The acquisition is done using the NUV imaging mode, either with Mirror A or Mirror B depending on the target surface brightness determined in a 9x9 pixel box. Based on the BOT with the GALEX catalog, visits 01,02,03,04,07 need mirror B.
Target Haro 11: the acquisition is done by a 2x2 spiral pattern ACQ/SEARCH and centering on the brightest pixel, followed by an ACQ/IMAGE. Taking the FUV flux within the COS aperture of 2e-14 erg/s/cm2/A, unresolved size, flat in f_lam, the S/N in mirror B of the PSA reaches ~40 in 30 seconds.
Other targets: the acquisition is done solely by an ACQ/IMAGE, as they have are very compact sources and have SDSS positions to about <0.4" accuracy. To calculate the acquisition times with MIRROR A, we used the COS ACQ ETC to estimate the time necessary to reach S/N~40 inside a 9x9 pixel box centered on the brightest part of the target. We do not know the intrinsic morphology good enough, so we make an optimistic and pessimistic guess: the optimistic guess is that half the FUV flux falls within the 9x9 pixels (this was true for some of our previous supercompact objects). The pessimistic guess is that the source is completely diffuse within the area given by the U-band half-light radius. Then, we chose the NUV acq-image exposure times such that in the pessimistic case we always have a S/N>30-35. In most cases, this will lead to am actually much higher S/N.
The MIRROR B acquisition times were calculated in a slightly different way: Because the Mirror B is so much less efficient, we risk wasting a lot of exposure time on acquisitions if our estimate for the 9x9 box surface brightness is way off. We assume that the central surface brightness for these targets is similar to that of our targets observed in Cycle 18, which had SB(9x9pixel) of ~16.5 mag. The ETC gives a mirror B acquisition time of ~400 seconds for a S/N=40. We will adopt these exposure times.
The table in the 'additional comments' field below gives the FUV magnitudes and surface brightness used to estimate acquisition and buffer times.
See numbers in the 'Additional comments' box below.
M(2.5") = FUV magnitude inside COS aperture
SB(ex) and SB(co) are the estimated surface brightness for the 9x9 pixel check box assuming that the source is completely extended (ex) and assuming it is compact (co). The last columns give the acquisition time and expected SNR in the completely extended source scenario. In most cases, the source will be more compact than that, and thus the SNR is expected to be higher in practice.
ID z M(2.5") SB(ex) SB(co) SB(used) MIRROR ACQTIME SNR ETC
===========================================================
Haro11 0.021 16.0 - - 14.1 B 30 >35 COS.ta.411443
J082354.95+280621.6 0.047 17.8 18.2 15.3 16.5 B 400 40 COS.ta.416436
J002101.02+005248 0.098 17.9 18.3 15.4 16.5 B 400 40 COS.ta.416436
J152521.84+075720.3 0.076 18.3 18.5 15.9 16.5 B 400 40 COS.ta.416436
J152141.52+075921.7 0.094 18.5 17.8 16.0 17.8 A 100 >40 COS.ta.411447
J141612.96+122340.5 0.123 18.7 18.3 16.2 18.3 A 100 >30 COS.ta.411445
J142856.4+165339.4 0.182 18.9 19.3 16.4 19.3 A 200 >30 COS.ta.411449
J114422.31+401221.2 0.127 18.9 18.9 16.4 18.9 A 200 >32 COS.ta.411450
J141454.23+054047.6 0.082 18.9 17.7 16.5 16.5 B 400 40 COS.ta.416436
J161245.59+081701 0.149 19.0 17.6 16.5 17.6 A 100 >40 COS.ta.411451
J111244.15+550347.1 0.1316 19.0 18.7 16.5 18.7 A 150 >30 COS.ta.411453
J102548.47+362258.4 0.127 19.0 19.3 16.6 19.3 A 200 >30 COS.ta.411449
J142947.03+064334.9 0.174 19.0 17.3 16.6 17.3 A 100 >50 COS.ta.411455
J111323.99+293039.2 0.175 19.5 19.6 17.0 19.6 A 300 >30 COS.ta.411457
ISM IN EXTERNAL GALAXIES
12
false
0.0
0.0
false
false
false
false
SUPPORTED
GALAXY
STARBURST
J2000
J2000
COS FUV flux 3.6e-15 erg/s/cm2/A, z = 0.047
GALAXY
STARBURST
J2000
J2000
COS FUV flux 3.2e-15 erg/s/cm2/A, z = 0.098
GALAXY
STARBURST
J2000
J2000
COS FUV flux 2.1e-15 erg/s/cm2/A, z = 0.076
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.8e-15 erg/s/cm2/A, z = 0.094
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.5e-15 erg/s/cm2/A, z = 0.12
GALAXY
STARBURST
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J2000
COS FUV flux 1.3e-15 erg/s/cm2/A, z = 0.18
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.3e-15 erg/s/cm2/A, z = 0.13
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.2e-15 erg/s/cm2/A, z = 0.08
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.2e-15 erg/s/cm2/A, z = 0.15
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.1e-15 erg/s/cm2/A, z = 0.13
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.1e-15 erg/s/cm2/A, z = 0.13
GALAXY
STARBURST
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J2000
COS FUV flux 1.1e-15 erg/s/cm2/A, z = 0.17
GALAXY
STARBURST
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J2000
COS FUV flux 7.3e-16 erg/s/cm2/A, z = 0.18
GALAXY
STARBURST
J2000
J2000
COS FUV flux 1.9e-14 erg/s/cm2/A, z = 0.021
COS/FUV
Spectroscopic
No
No
G130M
1291
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Spectroscopic
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G160M
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COS/FUV
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COS/FUV
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COS/FUV
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COS/FUV
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COS/FUV
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COS/FUV
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Spectroscopic
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No
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COS/FUV
Spectroscopic
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No
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COS/FUV
Spectroscopic
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No
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COS/FUV
Spectroscopic
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COS/FUV
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COS/FUV
Spectroscopic
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COS/FUV
Spectroscopic
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COS/FUV
Spectroscopic
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No
G130M
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COS/FUV
Spectroscopic
No
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true
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The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
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true
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The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
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true
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The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
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true
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The scheduling data was generated by CASM 20.2.
CASM was run in Phase II mode.
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true
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