J/ApJ/786/59 SED fitting results of HETDEX pilot survey (Hagen+, 2014)
Spectral energy distribution fitting of HETDEX pilot survey Lyα emitters
in COSMOS and GOODS-N.
Hagen A., Ciardullo R., Gronwall C., Acquaviva V., Bridge J., Zeimann G.R.,
Blanc G.A., Bond N.A., Finkelstein S.L., Song M., Gawiser E., Fox D.B.,
Gebhardt H., Malz A.I., Schneider D.P., Drory N., Gebhardt K., Hill G.J.
<Astrophys. J., 786, 59 (2014)>
=2014ApJ...786...59H 2014ApJ...786...59H (SIMBAD/NED BibCode)
ADC_Keywords: Energy distributions ; Galaxy catalogs ; Redshifts ; Reddening ;
Photometry, hydrogen-line ; Surveys
Keywords: cosmology: observations - galaxies: evolution -
galaxies: high-redshift - galaxies: starburst
Abstract:
We use broadband photometry extending from the rest-frame UV to the
near-IR to fit the individual spectral energy distributions of 63
bright (L(Lyα)>1043 erg/s) Lyα emitting galaxies
(LAEs) in the redshift range 1.9<z<3.6. We find that these LAEs
are quite heterogeneous, with stellar masses that span over three
orders of magnitude, from 7.5<log M/M☉<10.5. Moreover, although
most LAEs have small amounts of extinction, some high-mass objects
have stellar reddenings as large as E(B-V)∼0.4. Interestingly, in
dusty objects the optical depths for Lyα and the UV continuum
are always similar, indicating that Lyα photons are not
undergoing many scatters before escaping their galaxy. In contrast,
the ratio of optical depths in low-reddening systems can vary widely,
illustrating the diverse nature of the systems. Finally, we show that
in the star-formation-rate-log-mass diagram, our LAEs fall above the
"main-sequence" defined by z∼3 continuum selected star-forming
galaxies. In this respect, they are similar to submillimeter-selected
galaxies, although most LAEs have much lower mass.
Description:
The LAEs chosen for study were discovered with the George & Cynthia
Mitchell Spectrograph (previously known as VIRUS-P; Hill et al.
2008SPIE.7014E..70H 2008SPIE.7014E..70H) on the 2.7 m Harlan J. Smith Telescope during the
HPS (Adams et al. 2011, J/ApJS/192/5). This integral-field instrument,
which employs an array of 246 4.2" diameter fibers, covers ∼3 arcmin2
of sky at a time, and delivers 5 Å resolution spectra between the
wavelengths 3500 Å and 5800 Å. The HPS itself surveyed a total
of 169 arcmin2 in the COSMOS (Scoville et al. 2007ApJS..172....1S 2007ApJS..172....1S),
GOODS-N (Giavalisco et al. 2004ApJ...600L..93G 2004ApJ...600L..93G), MUNICS-S2 (Drory et al.
2001MNRAS.325..550D 2001MNRAS.325..550D), and XMM-LSS (Pierre et al. 2004JCAP....9...11P 2004JCAP....9...11P)
fields. The final HPS catalog consists of coordinates, redshifts,
R-band magnitudes, line fluxes, and equivalent widths for 397 emission-line
selected galaxies. Ninty-nine of these sources are non X-ray emitting
LAEs with 1.9<z<3.8, rest-frame equivalent widths EW0>20 Å, and
Lyα luminosities between 2.6x1042 and 1.1x1044 erg/s (Adams et al.
2011, J/ApJS/192/5; Blanc et al. 2011, J/ApJ/736/31). A total of 74 of
these HPS LAEs lie in the GOODS-N and COSMOS fields, where deep HST
data is available.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 75 63 SED Fitting Results
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See also:
J/A+A/498/13 : Lyman-α emitters from redshifts z∼2-3 (Nilsson+, 2009)
J/ApJ/736/31 : HETDEX pilot survey. II. 1.9<z<3.8 LAEs (Blanc+, 2011)
J/ApJS/192/5 : Emission-line galaxies from HETDEX pilot survey (Adams+, 2011)
J/ApJ/744/110 : LAE galaxies between 2.1=<z≤3.1 (Ciardullo+, 2012)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [HPS]
4- 6 I3 --- HPS [150/474] Galaxy identifier
( in Simbad)
8- 11 F4.2 --- z Redshift
13- 17 F5.2 [Msun] logM* Log of stellar mass
19- 22 F4.2 [Msun] E_logM* Upper limit uncertainty in logM*
24- 27 F4.2 [Msun] e_logM* Lower limit uncertainty in logM*
29- 32 F4.2 [yr] logAge Log of Age
34- 37 F4.2 [yr] E_logAge Upper limit uncertainty in logAge
39- 42 F4.2 [yr] e_logAge Lower limit uncertainty in logAge
44- 48 F5.3 --- E(B-V) Stellar reddening
50- 54 F5.3 --- E_E(B-V) Upper limit uncertainty in E(B-V)
56- 60 F5.3 --- e_E(B-V) Lower limit uncertainty in E(B-V)
62- 65 F4.2 kpc Rad Half-light radius
67- 70 F4.2 kpc e_Rad Error in Rad
72- 75 F4.1 --- chi2 Reduced χ2 value
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History:
From electronic version of the journal
(End) Prepared by Tiphaine Pouvreau [CDS] 20-Jun-2017