TY - JOUR
T1 - Correlation between star formation activity and electron density of ionized gas at z = 2.5
AU - Shimakawa, Rhythm
AU - Kodama, Tadayuki
AU - Steidel, Charles C.
AU - Tadaki, Ken ichi
AU - Tanaka, Ichi
AU - Strom, Allison L.
AU - Hayashi, Masao
AU - Koyama, Yusei
AU - Suzuki, Tomoko L.
AU - Yamamoto, Moegi
N1 - Publisher Copyright:
© 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2015/5/1
Y1 - 2015/5/1
N2 - In the redshift interval of 2 < z < 3, the physical conditions of the interstellar medium (ISM) in star-forming galaxies are likely to be different from those in the local Universe because of lower gaseous metallicities, higher gas fractions, and higher star formation activities. In fact, observations suggest that higher electron densities, higher ionization parameters, and harder UV radiation fields are common. In this paper, based on the spectra of H α-selected starforming galaxies at z = 2.5 taken with Multi-Object Spectrometer for InfraRed Exploration on Keck-1 telescope, we measure electron densities (ne) using the oxygen line ratio ([O II] λλ3726,3729), and investigate the relationships between the electron density of ionized gas and other physical properties. As a result, we find that the specific star formation rate (sSFR) and the surface density of SFR (ΣSFR) are correlated with the electron density at z =2.5 for the first time. The ΣSFR-ne relation is likely to be linked to the star formation law in HII regions (where star formation activity is regulated by interstellar pressure). Moreover, we discuss the mode of star formation in those galaxies. The correlation between sSFR and ΣSFR suggests that highly star-forming galaxies (with high sSFR) tend to be characterized by higher surface densities of star formation (ΣSFR) and thus higher ne values as well.
AB - In the redshift interval of 2 < z < 3, the physical conditions of the interstellar medium (ISM) in star-forming galaxies are likely to be different from those in the local Universe because of lower gaseous metallicities, higher gas fractions, and higher star formation activities. In fact, observations suggest that higher electron densities, higher ionization parameters, and harder UV radiation fields are common. In this paper, based on the spectra of H α-selected starforming galaxies at z = 2.5 taken with Multi-Object Spectrometer for InfraRed Exploration on Keck-1 telescope, we measure electron densities (ne) using the oxygen line ratio ([O II] λλ3726,3729), and investigate the relationships between the electron density of ionized gas and other physical properties. As a result, we find that the specific star formation rate (sSFR) and the surface density of SFR (ΣSFR) are correlated with the electron density at z =2.5 for the first time. The ΣSFR-ne relation is likely to be linked to the star formation law in HII regions (where star formation activity is regulated by interstellar pressure). Moreover, we discuss the mode of star formation in those galaxies. The correlation between sSFR and ΣSFR suggests that highly star-forming galaxies (with high sSFR) tend to be characterized by higher surface densities of star formation (ΣSFR) and thus higher ne values as well.
KW - Galaxies: ISM
KW - Galaxies: formation
KW - Galaxies: high-redshift
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U2 - 10.1093/mnras/stv915
DO - 10.1093/mnras/stv915
M3 - Article
AN - SCOPUS:84938150616
SN - 0035-8711
VL - 451
SP - 1284
EP - 1289
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -