PHYSICAL PROPERTIES OF Ly{alpha} EMITTERS AT z {approx} 0.3 FROM UV-TO-FIR MEASUREMENTS

Journal Article · Fri Jun 01 00:00:00 EDT 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/751/2/139· OSTI ID:22037145

Oteo, I; Bongiovanni, A; Perez Garcia, A M; Cepa, J; Pintos-Castro, I ^[1]; Ederoclite, A ^[2]; Sanchez-Portal, M; Altieri, B ^[3]; Perez-Martinez, R ^[4]; Lutz, D; Berta, S; Foerster Schreiber, N; Genzel, R; Magnelli, B ^[5]; Andreani, P ^[6]; Aussel, H; Daddi, E; Elbaz, D; Le Floc'h, E ^[7]; Cimatti, A ^[8] ; others, and

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1. Instituto de Astrofisica de Canarias (IAC), E-38200 La Laguna, Tenerife (Spain)
2. Centro de Estudios de Fisica del Cosmos de Aragon, Plaza San Juan 1, Planta 2, Teruel, 44001 (Spain)
3. Herschel Science Centre (ESAC), Villafranca del Castillo (Spain)
4. XMM/Newton Science Operations Centre (ESAC), Villafranca del Castillo (Spain)
5. Max-Planck-Institut fuer Extraterrestrische Physik (MPE), Postfach 1312, 85741 Garching (Germany)
6. ESO, Karl-Schwarzchild-Str. 2, D-85748 Garching (Germany)
7. Commissariat a l'Energie Atomique (CEA-SAp) Saclay (France)
8. Dipartimento di Astronomia, Universita di Bologna, Via Ranzani 1, 40127 Bologna (Italy)

The analysis of the physical properties of low-redshift Ly{alpha} emitters (LAEs) can provide clues in the study of their high-redshift analogs. At z {approx} 0.3, LAEs are bright enough to be detected over almost the entire electromagnetic spectrum and it is possible to carry out a more precise and complete study than at higher redshifts. In this work, we examine the UV and IR emission, dust attenuation, star formation rate (SFR), and morphology of a sample of 23 GALEX-discovered star-forming LAEs at z {approx} 0.3 with direct UV (GALEX), optical (ACS), and FIR (PACS and MIPS) data. Using the same UV and IR limiting luminosities, we find that LAEs at z {approx} 0.3 tend to be less dusty, have slightly higher total SFRs, have bluer UV continuum slopes, and are much smaller than other galaxies that do not exhibit Ly{alpha} emission in their spectrum (non-LAEs). These results suggest that at z {approx} 0.3, Ly{alpha} photons tend to escape from small galaxies with low dust attenuation. Regarding their morphology, LAEs belong to Irr/merger classes, unlike non-LAEs. Size and morphology represent the most noticeable difference between LAEs and non-LAEs at z {approx} 0.3. Furthermore, the comparison of our results with those obtained at higher redshifts indicates either that the Ly{alpha} technique picks up different kind of galaxies at different redshifts or that the physical properties of LAEs are evolving with redshift.

• OSTI ID: 22037145
• Journal Information: Astrophysical Journal, Vol. 751, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ASTRONOMY
ASTROPHYSICS
COMPARATIVE EVALUATIONS
COSMIC DUST
COSMIC PHOTONS
EMISSION SPECTRA
FAR INFRARED RADIATION
GALACTIC EVOLUTION
GALAXIES
INFRARED SPECTRA
LUMINOSITY
MORPHOLOGY
PHOTON EMISSION
RED SHIFT
STARS
ULTRAVIOLET RADIATION