The ultraviolet luminosity function of star-forming galaxies between redshifts of 0.4 and 0.6

被引：0

作者：

Page, M. J. ^{[1
]}

Dwelly, T. ^{[2
]}

Mchardy, I ^{[3
]}

Seymour, N. ^{[4
]}

Mason, K. O. ^{[5
]}

Sharma, M. ^{[1
]}

Kennea, J. A. ^{[6
]}

Sasseen, T. P. ^{[7
]}

Breeveld, A. A. ^{[1
]}

Matthews, A. E. ^{[1
]}

机构：

[1] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England

[2] Tdastro Com, Camden Rd, Bath BA1 5JD, England

[3] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, England

[4] Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia

[5] Satellite Applicat Catapult, Fermi Ave,Harwell Campus, Didcot OX11 0QR, Oxon, England

[6] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[7] Tyto Athene, 5383 Hollister Ave, Santa Barbara, CA 93111 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 536卷 / 01期

关键词：

galaxies: evolution; galaxies: luminosity function; mass function; ultraviolet: galaxies; FORMATION RATE DENSITY; FAINT-END SLOPE; UV-CONTINUUM; DEEP FIELD; PHOTOMETRIC REDSHIFTS; FORMATION HISTORY; DYNAMIC-RANGE; EVOLUTION; CALIBRATION; SPECTRA;

D O I：

10.1093/mnras/stae2498

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We combine ultraviolet imaging of the 13(H) survey field, taken with the XMM-Newton Optical Monitor telescope (XMM-OM) and the Neil Gehrels Swift Observatory Ultraviolet and Optical Telescope (UVOT) in the UVM2 band, to measure rest-frame ultraviolet 1500 & Aring; luminosity functions of star-forming galaxies with redshifts z between 0.4 and 0.6. In total the UVM2 imaging covers a sky area of 641 arcmin(2), and we detect 273 galaxies in the UVM2 image with 0.4 < z < 0.6. The luminosity function is fit by a Schechter function with best-fitting values for the faint end slope alpha = -1.8(-0.3)(+0.4) and characteristic absolute magnitude M-& lowast; = -19.1(-0.4)(+0.3). In common with XMM-OM based studies at higher redshifts, our best-fitting value for M & lowast; is fainter than previous measurements. We argue that the purging of active galactic nuclei from the sample, facilitated by the cospatial X-ray survey carried out with XMM-Newton is important for the determination of M & lowast;. At the brightest absolute magnitudes (M-1500<-18.5), the average UV colour of our galaxies is consistent with that of minimal-extinction local analogues, but the average UV colour is redder for galaxies at fainter absolute magnitudes, suggesting that higher levels of dust attenuation enter the sample at absolute magnitudes somewhat fainter than M-& lowast;.

引用

页码：518 / 529

页数：12