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Star Formation in Emission-Line Galaxies Between Redshifts of 0.8 and 1.6 | Erin K.S. Hicks
; Matthew A. Malkan
; Harry I. Teplitz
; Patrick J. McCarthy
; Lin Yan
; | Date: |
30 Aug 2002 | Journal: | Astrophys.J. 581 (2002) 205-222 | Subject: | astro-ph | Affiliation: | University of California, Los Angeles, NASA Goddard Space Flight Center, Observatories of the Carnegie Institution of Washington, SIRTF Science Center, California Institute of Technology | Abstract: | Optical spectra of 14 emission-line galaxies representative of the 1999 NICMOS parallel grism Ha survey of McCarthy et al. are presented. Of the 14, 9 have emission lines confirming the redshifts found in the grism survey. The higher resolution of our optical spectra improves the redshift accuracy by a factor of 5. The [O II]/Ha values of our sample are found to be more than two times lower than expected from Jansen et al. This [O II]/Ha ratio discrepancy is most likely explained by additional reddening in our Ha-selected sample [on average, as much as an extra E(B-V) = 0.6], as well as to a possible stronger dependence of the [O II]/Ha ratio on galaxy luminosity than is found in local galaxies. The result is that star formation rates (SFRs) calculated from [O II]3727 emission, uncorrected for extinction, are found to be on average 4 +/- 2 times lower than the SFRs calculated from Ha emission. Classification of emission-line galaxies as starburst or Seyfert galaxies based on comparison of the ratios [O II]/Hb and [Ne III]3869/Hb is discussed. New Seyfert 1 diagnostics using the Ha line luminosity, H-band absolute magnitude, and Ha equivalent widths are also presented. One galaxy is classified as a Seyfert 1 based on its broad emission lines, implying a comoving number density for Seyfert 1s of 2.5{+5.9, -2.1} times 10^{-5} Mpc^{-3}. This commoving number density is a factor of 2.4{+5.5,-2.0} times higher than estimated by other surveys. | Source: | arXiv, astro-ph/0208551 | Services: | Forum | Review | PDF | Favorites |
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