Strong Nebular Line Ratios in the Spectra of z~2-3 Star-forming Galaxies: First Results from KBSS-MOSFIRE
We present initial results of a deep near-IR spectroscopic survey covering the 15 fields of the Keck Baryonic Structure Survey (KBSS) using MOSFIRE on the Keck 1 telescope, focusing on a sample of 251 galaxies with redshifts 2.0< z < 2.6, star-formation rates 2 < SFR < 200 M_sun/yr, and...
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creator | Steidel, C C Rudie, G C Strom, A L Pettini, M Reddy, N A Shapley, A E Trainor, R F Erb, D K Turner, M L Konidaris, N P Kulas, K R Mace, G Matthews, K McLean, I S |
description | We present initial results of a deep near-IR spectroscopic survey covering the 15 fields of the Keck Baryonic Structure Survey (KBSS) using MOSFIRE on the Keck 1 telescope, focusing on a sample of 251 galaxies with redshifts 2.0< z < 2.6, star-formation rates 2 < SFR < 200 M_sun/yr, and stellar masses 8.6 < log(M*/M_sun) < 11.4, with high-quality spectra in both H- and K-band atmospheric windows. We show unambiguously that the locus of z~2.3 galaxies in the "BPT" nebular diagnostic diagram exhibits a disjoint, yet similarly tight, relationship between the ratios [NII]6585/Halpha and [OIII]/Hbeta as compared to local galaxies. Using photoionization models, we argue that the offset of the z~2.3 locus relative to z~ 0 is explained by a combination of harder ionizing radiation field, higher ionization parameter, and higher N/O at a given O/H than applies to most local galaxies, and that the position of a galaxy along the z~2.3 star-forming BPT locus is surprisingly insensitive to gas-phase oxygen abundance. The observed nebular emission line ratios are most easily reproduced by models in which the net ionizing radiation field resembles a blackbody with effective temperature T_eff = 50000-60000 K and N/O close to the solar value at all O/H. We critically assess the applicability of commonly-used strong line indices for estimating gas-phase metallicities, and consider the implications of the small intrinsic scatter in the empirical relationship between excitation-sensitive line indices and stellar mass (i.e., the "mass-metallicity" relation), at z~2.3. |
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We show unambiguously that the locus of z~2.3 galaxies in the "BPT" nebular diagnostic diagram exhibits a disjoint, yet similarly tight, relationship between the ratios [NII]6585/Halpha and [OIII]/Hbeta as compared to local galaxies. Using photoionization models, we argue that the offset of the z~2.3 locus relative to z~ 0 is explained by a combination of harder ionizing radiation field, higher ionization parameter, and higher N/O at a given O/H than applies to most local galaxies, and that the position of a galaxy along the z~2.3 star-forming BPT locus is surprisingly insensitive to gas-phase oxygen abundance. The observed nebular emission line ratios are most easily reproduced by models in which the net ionizing radiation field resembles a blackbody with effective temperature T_eff = 50000-60000 K and N/O close to the solar value at all O/H. We critically assess the applicability of commonly-used strong line indices for estimating gas-phase metallicities, and consider the implications of the small intrinsic scatter in the empirical relationship between excitation-sensitive line indices and stellar mass (i.e., the "mass-metallicity" relation), at z~2.3.]]></description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1405.5473</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Abundance ; Astronomical models ; Atmospheric models ; Atmospheric windows ; Black body radiation ; Blackbody ; Diagnostic systems ; Galaxies ; Ionization ; Ionizing radiation ; Line spectra ; Loci ; Metallicity ; Near infrared radiation ; Photoionization ; Physics - Astrophysics of Galaxies ; Physics - Cosmology and Nongalactic Astrophysics ; Star & galaxy formation ; Star formation ; Stellar mass</subject><ispartof>arXiv.org, 2014-09</ispartof><rights>2014. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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We show unambiguously that the locus of z~2.3 galaxies in the "BPT" nebular diagnostic diagram exhibits a disjoint, yet similarly tight, relationship between the ratios [NII]6585/Halpha and [OIII]/Hbeta as compared to local galaxies. Using photoionization models, we argue that the offset of the z~2.3 locus relative to z~ 0 is explained by a combination of harder ionizing radiation field, higher ionization parameter, and higher N/O at a given O/H than applies to most local galaxies, and that the position of a galaxy along the z~2.3 star-forming BPT locus is surprisingly insensitive to gas-phase oxygen abundance. The observed nebular emission line ratios are most easily reproduced by models in which the net ionizing radiation field resembles a blackbody with effective temperature T_eff = 50000-60000 K and N/O close to the solar value at all O/H. We critically assess the applicability of commonly-used strong line indices for estimating gas-phase metallicities, and consider the implications of the small intrinsic scatter in the empirical relationship between excitation-sensitive line indices and stellar mass (i.e., the "mass-metallicity" relation), at z~2.3.]]></description><subject>Abundance</subject><subject>Astronomical models</subject><subject>Atmospheric models</subject><subject>Atmospheric windows</subject><subject>Black body radiation</subject><subject>Blackbody</subject><subject>Diagnostic systems</subject><subject>Galaxies</subject><subject>Ionization</subject><subject>Ionizing radiation</subject><subject>Line spectra</subject><subject>Loci</subject><subject>Metallicity</subject><subject>Near infrared radiation</subject><subject>Photoionization</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Cosmology and Nongalactic Astrophysics</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stellar mass</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkE1PAjEARBsTEwly92SaeF7sJ63elAASURLqfdMtrZYsW2y7BD34213E01zeTCYPgCuMhkxyjm51PPj9EDPEh5wJegZ6hFJcSEbIBRiktEEIkZEgnNMe8CrH0LzDV1u1tY5w4RsLVzr7kKBvYP6wUO2syVHD4OD3DykoVFnHwoW49V1xpmt98Dbdw6mPKcOVTW2dE3QxbOHzo1LFy1JN56vJJTh3uk528J99oKaTt_FTsVjO5uOHRaE5ZoXEHFVmLTlasxG9I0ZU0gmpBWXOWoO0Ns5io2lVrYkwlRRiZCyiDDveBe2D69Pqn4VyF_1Wx6_yaKM82uiAmxOwi-GztSmXm9DGpntUEiQpRoIiRn8BgPFhag</recordid><startdate>20140919</startdate><enddate>20140919</enddate><creator>Steidel, C C</creator><creator>Rudie, G C</creator><creator>Strom, A L</creator><creator>Pettini, M</creator><creator>Reddy, N A</creator><creator>Shapley, A E</creator><creator>Trainor, R F</creator><creator>Erb, D K</creator><creator>Turner, M L</creator><creator>Konidaris, N P</creator><creator>Kulas, K R</creator><creator>Mace, G</creator><creator>Matthews, K</creator><creator>McLean, I S</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20140919</creationdate><title>Strong Nebular Line Ratios in the Spectra of z~2-3 Star-forming Galaxies: First Results from KBSS-MOSFIRE</title><author>Steidel, C C ; Rudie, G C ; Strom, A L ; Pettini, M ; Reddy, N A ; Shapley, A E ; Trainor, R F ; Erb, D K ; Turner, M L ; Konidaris, N P ; Kulas, K R ; Mace, G ; Matthews, K ; McLean, I S</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a514-8150bcd850d46392c7b8f78a734feec0aacfe1ca3bbd27cb8776ce0341f5e033</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Abundance</topic><topic>Astronomical models</topic><topic>Atmospheric models</topic><topic>Atmospheric windows</topic><topic>Black body radiation</topic><topic>Blackbody</topic><topic>Diagnostic systems</topic><topic>Galaxies</topic><topic>Ionization</topic><topic>Ionizing radiation</topic><topic>Line spectra</topic><topic>Loci</topic><topic>Metallicity</topic><topic>Near infrared radiation</topic><topic>Photoionization</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Cosmology and Nongalactic Astrophysics</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stellar mass</topic><toplevel>online_resources</toplevel><creatorcontrib>Steidel, C C</creatorcontrib><creatorcontrib>Rudie, G C</creatorcontrib><creatorcontrib>Strom, A L</creatorcontrib><creatorcontrib>Pettini, M</creatorcontrib><creatorcontrib>Reddy, N A</creatorcontrib><creatorcontrib>Shapley, A E</creatorcontrib><creatorcontrib>Trainor, R F</creatorcontrib><creatorcontrib>Erb, D K</creatorcontrib><creatorcontrib>Turner, M L</creatorcontrib><creatorcontrib>Konidaris, N P</creatorcontrib><creatorcontrib>Kulas, K R</creatorcontrib><creatorcontrib>Mace, G</creatorcontrib><creatorcontrib>Matthews, K</creatorcontrib><creatorcontrib>McLean, I S</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Access via ProQuest (Open Access)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Steidel, C C</au><au>Rudie, G C</au><au>Strom, A L</au><au>Pettini, M</au><au>Reddy, N A</au><au>Shapley, A E</au><au>Trainor, R F</au><au>Erb, D K</au><au>Turner, M L</au><au>Konidaris, N P</au><au>Kulas, K R</au><au>Mace, G</au><au>Matthews, K</au><au>McLean, I S</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Strong Nebular Line Ratios in the Spectra of z~2-3 Star-forming Galaxies: First Results from KBSS-MOSFIRE</atitle><jtitle>arXiv.org</jtitle><date>2014-09-19</date><risdate>2014</risdate><eissn>2331-8422</eissn><abstract><![CDATA[We present initial results of a deep near-IR spectroscopic survey covering the 15 fields of the Keck Baryonic Structure Survey (KBSS) using MOSFIRE on the Keck 1 telescope, focusing on a sample of 251 galaxies with redshifts 2.0< z < 2.6, star-formation rates 2 < SFR < 200 M_sun/yr, and stellar masses 8.6 < log(M*/M_sun) < 11.4, with high-quality spectra in both H- and K-band atmospheric windows. We show unambiguously that the locus of z~2.3 galaxies in the "BPT" nebular diagnostic diagram exhibits a disjoint, yet similarly tight, relationship between the ratios [NII]6585/Halpha and [OIII]/Hbeta as compared to local galaxies. Using photoionization models, we argue that the offset of the z~2.3 locus relative to z~ 0 is explained by a combination of harder ionizing radiation field, higher ionization parameter, and higher N/O at a given O/H than applies to most local galaxies, and that the position of a galaxy along the z~2.3 star-forming BPT locus is surprisingly insensitive to gas-phase oxygen abundance. The observed nebular emission line ratios are most easily reproduced by models in which the net ionizing radiation field resembles a blackbody with effective temperature T_eff = 50000-60000 K and N/O close to the solar value at all O/H. We critically assess the applicability of commonly-used strong line indices for estimating gas-phase metallicities, and consider the implications of the small intrinsic scatter in the empirical relationship between excitation-sensitive line indices and stellar mass (i.e., the "mass-metallicity" relation), at z~2.3.]]></abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1405.5473</doi><oa>free_for_read</oa></addata></record> |
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subjects | Abundance Astronomical models Atmospheric models Atmospheric windows Black body radiation Blackbody Diagnostic systems Galaxies Ionization Ionizing radiation Line spectra Loci Metallicity Near infrared radiation Photoionization Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Star & galaxy formation Star formation Stellar mass |
title | Strong Nebular Line Ratios in the Spectra of z~2-3 Star-forming Galaxies: First Results from KBSS-MOSFIRE |
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