J/MNRAS/506/473 UV luminosity functions of SFR galaxies (Page+, 2021)
The ultraviolet luminosity function of star-forming galaxies between
redshifts of 0.6 and 1.2.
Page M.J., Dwelly T., McHardy I., Seymour N., Mason K.O., Sharma M.,
Kennea J.A., Sasseen T.P., Rawlings J.I., Breeveld A.A., Ferreras I.,
Loaring N.S., Walton D.J., Symeonidis M.
<Mon. Not. R. Astron. Soc., 506, 473-487 (2021)>
=2021MNRAS.506..473P 2021MNRAS.506..473P (SIMBAD/NED BibCode)
ADC_Keywords: X-ray sources ; Galaxies ; Star Forming Region ;
Active gal. nuclei ; Redshifts ; Photometry, ultraviolet
Keywords: galaxies: evolution - galaxies: luminosity function, mass function -
ultraviolet: galaxies
Abstract:
We use ultraviolet (UV) imaging taken with the XMM-Newton Optical
Monitor telescope (XMM-OM), covering 280 arcmin2 in the UVW1 band
(λeff = 2910 Å) to measure rest-frame UV 1500-Å
luminosity functions of galaxies with redshifts z between 0.6 and 1.2.
The XMM-OM data are supplemented by a large body of optical and
infrared imaging to provide photometric redshifts. The XMM-OM data
have a significantly narrower point spread function (resulting in less
source confusion) and simpler K-correction than the GALEX data
previously employed in this redshift range. UV-bright active galactic
nuclei are excluded to ensure that the luminosity functions relate
directly to the star-forming galaxy population. Binned luminosity
functions and parametric Schechter-function fits are derived in two
redshift intervals: 0.6 < z < 0.8 and 0.8 < z < 1.2. We find that the
luminosity function evolves such that the characteristic absolute
magnitude M* is brighter for 0.8 < z < 1.2 than for 0.6 < z < 0.8.
Description:
We use an observation of the 13H XMM-Newton Deep Field (McHardy et
al. 2003MNRAS.342..802M 2003MNRAS.342..802M, Cat. J/MNRAS/342/802; Loaring et al.
2005MNRAS.362.1371L 2005MNRAS.362.1371L, Cat. J/MNRAS/362/1371) taken with the
XMM-Newton Optical Monitor (XMM-OM; Mason et al.
2001A&A...365L..36M 2001A&A...365L..36M) through the UVW1 filter, which has an effective
wavelength of 2910 Å, to examine the UV luminosity function of
galaxies in the redshift interval 0.6 < z < 1.2. The 13H Field is
centred at 13h34m30s +37 53' (J2000), and corresponds to an area
of exceptionally low Galactic extinction (E(B - V) = 0.005 mag;
Schlafly & Finkbeiner 2011ApJ...737..103S 2011ApJ...737..103S). This low extinction, and
the availability of redshifts facilitated by extensive multiwavelength
follow-up, make the 13H Field an excellent location for a study of the
UV galaxy luminosity function. We describe the optical and infrared
imaging of the 13H Field and the techniques that were used to derive
photometric redshifts. This material serves also as a reference for
the data and techniques used in earlier works on the 13H Field that
make use of these photometric redshifts (Seymour et al.
2009MNRAS.398.1573S 2009MNRAS.398.1573S, 2010MNRAS.402.2666S 2010MNRAS.402.2666S; Symeonidis et al.
2009MNRAS.397.1728S 2009MNRAS.397.1728S).
Based on previous spectroscopic and photometric observations,
as we detail in sections 2.2 and 2.3 respectively.
We details observations data reductions and analyses used for
photometric redshifts determination in order to compare them to
spectroscopic redshifts (see sections 2.3.1 - 2.8).
Hereafter, we match the UVW1 sources to counterparts in the optical,
we have used our deep imaging in Johnson B taken with the SuprimeCam
on the Subaru Telescope (see Section 2.3.2). Finally, we proceed to
exclusion of broad-line AGN candidates (see section 2.10) and to
corrections such as galactic extinction and K-correction (see sections
3.2 and 3.3 respectively). Giving us the sample of 133 UVW1-selected
galaxies used to construct the luminosity functions as the
table3.dat shoes.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 48 133 *UVW1-selected galaxies used to construct
the luminosity functions
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Note on table3.dat: Magnitudes are given in the AB system (Oke & Gunn
1983ApJ...266..713O 1983ApJ...266..713O). We have assumed cosmological parameters
H0 = 70 km/s/Mpc, ΩΛ = 0.7, and Ωm = 0.3.
Unless stated otherwise, uncertainties are given at 1σ.
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See also:
J/MNRAS/342/802 : Chandra survey of 13-h XMM/ROSAT survey (McHardy+, 2003)
J/MNRAS/362/1371 : XMM-Newton 13H deep field (Loaring+, 2005)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh Right ascension (J2000)
4- 5 I2 min RAm Right ascension (J2000)
7- 11 F5.2 s RAs [] Right ascension (J2000)
13 A1 --- DE- Sign of declination (J2000)
14- 15 I2 deg DEd Declination (J2000)
17- 18 I2 arcmin DEm Declination (J2000)
20- 23 F4.1 arcsec DEs Declination (J2000)
25- 30 F6.3 mag UVW1mag Apparent AB magnitude in UVW1 filter at an
effective wavelength of 2910 Å (UVW1mag)
32- 36 F5.3 mag e_UVW1mag Mean error of UVW1mag (eUVW1mag_)
38- 42 F5.3 --- z Measured redshift (z)
44- 48 A5 --- f_z [spec phot] Indicates whether the redshift is
derived from spectroscopic or photometric data
(spec/phot)
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 20-Jun-2024