0
Assigned ID: 27
----- Attempting Submission 1 (Mon Jul 30 15:32:20 GMT 2018) -----
HST Phase I Proposal 27 (LyC3_submitted.apt) successfully submitted.
Receipt: # 27-1
----- Attempting Submission 2 (Wed Aug 01 06:36:11 GMT 2018) -----
HST Phase I Proposal 27 (LyC3_submitted.apt) successfully submitted.
Receipt: # 27-2
----- Attempting Submission 3 (Sat Aug 04 04:58:48 GMT 2018) -----
HST Phase I Proposal 27 (LyC3_submitted.apt) successfully submitted.
Receipt: # 27-3
----- Attempting Submission 4 (Thu Aug 16 09:20:36 GMT 2018) -----
0
----- Attempting Submission 1 (Fri Nov 16 17:49:04 GMT 2018) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 2 (Wed Dec 12 17:40:28 GMT 2018) -----
Lyman continuum leakage in z~0.3 - 0.4 dwarf compact star-forming galaxies with stellar masses < 1.e8 Msun
One of the key questions in observational cosmology is the identification of the sources responsible for cosmic reionization. The general consensus is that a population of faint low-mass galaxies must be responsible for the bulk of the ionizing photons. However, until recently, attempts at identifying individual galaxies showing Lyman continuum (LyC) leakage have only found very few such galaxies, both at high and low redshifts. A breakthrough was recently achieved by Izotov et al. (2016ab, 2018ab), who detected LyC emission in eleven out of eleven low-redshift (z~0.3) compact star-forming galaxies (SFG) with LyC escape fractions of 2-72%, using HST/COS observations. However, all these galaxies have relatively high stellar masses > 1e8 solar masses while it is generally thought that the lower mass galaxies were the main sources of the reionization of the Universe. It is proposed here to extend previous studies to nine compact SFGs at z~0.3-0.4 with lower stellar masses in the range ~2e7 - 1e8 Msun, a range which has not been explored by HST/COS. This will allow to determine if they are also LyC leakers and if the LyC escape fraction continues to rise with decreasing stellar masses. Finally the requested COS observations will allow for the determination of the Lyman alpha line profile of these objects, providing thus an empirical probe of this indirect LyC leakage indicator. Since the low-mass compact SFGs share many properties with typical SFGs at high redshift this study will provide important insight on the sources of cosmic reionization.
The nine selected galaxies are sufficiently faint to satisfy safety conditions for observing with the COS. Furthermore, there are no sources brighter than the COS safety limits in circular regions with the diameter of 43 arcsec centered on the selected galaxies.
In all exposure time calculations the angular galaxy radius is chosen to be 0.2 arcsec, inside which most of the galaxy light is concentrated.
NUV acquisition images of the targets will be obtained with the standard Mirror A and the AQN/IMAGE mode, with exposures of ~800 - 900 seconds to reach a S/N~20 inside a 9x9 pixel box centered on the brightest part of the galaxy. The GALEX NUV magnitudes were adopted to estimate S/N, excluding J1121+3806, for which the GALEX NUV magnitude is absent and it was estimated from extrapolation of the SED using SDSS optical spectrum. This object is seen in the DSS. The total time for acquisition is up to 120s+2x900s=1920s per object (HST Primer manual), or ~2/3 orbit. As a bonus, it will be possible to study the UV morphology of the selected objects with these images.
The COS will be used in combination with the following 2 gratings:
1) the medium-resolution G160M grating to observe the Ly-alpha line with the resolution better than ~50 km/s, sufficient to separate blue and red peaks. The required number of orbits to obtain a S/N>2-4 of the continuum near Ly-alpha line for a 100-pixel binned spectrum is derived adopting a flux density at the wavelength 1216x(1+z) obtained from the SED fit of the optical spectrum. This exposure would be enough to obtain the Ly-alpha profile with a sufficient accuracy for measurements of
peak separation and radiative transfer modeling;
2) the low-resolution G140L grating centered at 800A to measure the LyC. The required number of orbits for each object is calculated so as to detect the LyC at the level above 3sigma with a 400-pixel binning of the data at the observed wavelength 912x(1+z). For the LyC, the escape fraction of approximately 10% and the intrinsic LyC flux density obtained from the relation I(Hbeta)/I(912) = 9 A are adopted, where I(Hbeta) is the extinction-corrected flux of the Hbeta emission line.
For each target are needed ~2/3 orbit for acquisition, ~1.3 orbit for the spectrum with the medium-resolution G160M grating, and 3 orbits for the spectrum with the low-resolution G140L grating, totalling 5 orbits per object. We request a total of 45 orbits for 9 objects.
Galaxies and the IGM
Cosmology
6
false
false
true
false
false
false
false
SUPPORTED
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
NUV=21.25+/-0.02, I(912)=4e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1765A)=4e-17
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
FUV=22.05+/-0.29, NUV=21.92+/-0.12, I(912)=8e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1709A)=3e-17
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
FUV=20.92+/-0.37, NUV=21.29+/-0.35, I(912)=7e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1698A)=1.1e-16
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
FUV=21.53+/-0.20, NUV=21.72+/-0.20, I(912)=6e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1603A)=5.5e-17
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
NUV=22.22+/-0.39, I(912)=6e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1608A)=4e-17
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
NUV=21.91+/-0.12, I(912)=8e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1729A)=5e-17
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
NUV=21.60+/-0.14, I(912)=4e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1658A)=4e-17
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
NUV=21.13+/-0.10, I(912)=9e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1660A)=1.1e-16
GALAXY
DWARF COMPACT
STARBURST
NO
The object is compact. The coordinates of the brightest pixel were measured with Aladin v8.0 using SDSS images.
J2000
J2000
FUV=21.52+/-0.39, NUV=21.70+/-0.39, I(912)=7e-18 (~10 percent of the intrinsic flux), I(1216x(1+z))=I(1663A)=6.5e-17
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1533
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1600
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1533
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1533
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1623
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1577
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1589
COS/FUV
Spectroscopic
No
No
G140L
800
COS/FUV
Spectroscopic
No
No
G160M
1577
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