2024RNAAS...8..266G

Query : 2024RNAAS...8..266G

2024RNAAS...8..266G - Research Notes of the AAS, 8, 266 (2024/October-0)

Emission-line Ratios and Ionization Conditions of CEERS Star-forming Galaxies with JWST/NIRSpec.

GUPTA A.R., KIRKPATRICK A., FERNANDEZ V., ARRABAL HARO P., BACKHAUS B.E., CLERI N.J., GROGIN N.A. and KOEKEMOER A.M.

Abstract (from CDS):

Galaxy emission-line fluxes can constrain star formation rates (SFRs) and interstellar medium (ISM) ionization. We investigate rest-frame optical emission lines of 71 star-forming galaxies (SFGs) at redshift 0.7 < z < 7 using JWST/NIRSpec measurements from the Cosmic Evolution Early Release Science survey. We use Hα to measure SFR and utilize Hubble Space Telescope CANDELS stellar mass estimates to determine specific SFR (sSFR) and compare with the SFG main sequence (MS). We create [O III]λ5008/Hβ versus [Ne III]λ3870/[O II]λ3728 line ratio diagrams. The line ratios appear to correlate with sSFR, and our results suggest that sSFR is the parameter that governs ionization conditions rather than SFR or a galaxy's distance from the MS. These measurements reveal a rich diversity of ISM conditions and physical galaxy properties throughout cosmic time.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Galaxy evolution - Emission line galaxies - Active galaxies

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME Extended Groth Strip reg 14 19 +52.8           ~ 1023 0

Query : 2024RNAAS...8..266G

Basic data :
NAME Extended Groth Strip -- Region defined in the Sky
Other object types: otypes_help 		reg ()
ICRS coord. (ep=J2000) : 		14 19 00.0 +52 48 00 [ ] E ~
FK4 coord. (ep=B1950 eq=1950) : 		14 17 16.3 +53 01 45 [ ]
Gal coord. (ep=J2000) : 		096.4814 +59.5977 [ ]
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Identifiers (2) :
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NAME EGS NAME Extended Groth Strip

References (1023 between 1850 and 2026) (Total 1023)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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Herschel : 31   

   

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