Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies

IF 4.8 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS
Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
{"title":"Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies","authors":"Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu","doi":"10.3847/1538-4357/acf466","DOIUrl":null,"url":null,"abstract":"Abstract We study ultraviolet H i and metal-line transitions in the circumgalactic medium (CGM) of 15 massive, quenched luminous red galaxies (LRGs) at redshift z ∼ 0.5 and with impact parameters up to 400 kpc. We selected eight LRG–CGM systems to study general properties of the CGM around LRGs, while the other seven are already known to contain cool CGM gas from Mg ii optical studies (Mg ii -LRGs). In the general LRG population, we detect H i in four of eight LRGs, in all cases with N H I < 10 16.7 cm −2 . In contrast, all Mg ii -LRGs show H i ; for four LRGs, the H i column density is N H I ≳ 10 18 cm −2 . The CGM of LRGs also shows low and intermediate ionized lines (such as C iii , C ii , Si iii , and Si ii ) and highly ionized lines of O vi (we detect O vi around five of seven Mg ii -LRGs and one of eight in the random sample). Next, we combine our sample with literature LRGs and ≲ L * galaxies, and we find that while for ≲ L * galaxies CGM H i Ly α absorption is stronger as galaxies are more massive, the cool CGM traced by H i Ly α is suppressed above stellar masses of M * ∼ 10 11.5 M ☉ . While most LRG–CGM systems show weak or nondetectable O vi (equivalent width < 0.2 Å), a few LRG–CGM systems show strong O vi 1031, which in most cases likely originates from groups containing both an LRG and a blue star-forming neighboring galaxy.","PeriodicalId":50735,"journal":{"name":"Astrophysical Journal","volume":null,"pages":null},"PeriodicalIF":4.8000,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":null,"platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astrophysical Journal","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/10.3847/1538-4357/acf466","RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q1","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0

Abstract

Abstract We study ultraviolet H i and metal-line transitions in the circumgalactic medium (CGM) of 15 massive, quenched luminous red galaxies (LRGs) at redshift z ∼ 0.5 and with impact parameters up to 400 kpc. We selected eight LRG–CGM systems to study general properties of the CGM around LRGs, while the other seven are already known to contain cool CGM gas from Mg ii optical studies (Mg ii -LRGs). In the general LRG population, we detect H i in four of eight LRGs, in all cases with N H I < 10 16.7 cm −2 . In contrast, all Mg ii -LRGs show H i ; for four LRGs, the H i column density is N H I ≳ 10 18 cm −2 . The CGM of LRGs also shows low and intermediate ionized lines (such as C iii , C ii , Si iii , and Si ii ) and highly ionized lines of O vi (we detect O vi around five of seven Mg ii -LRGs and one of eight in the random sample). Next, we combine our sample with literature LRGs and ≲ L * galaxies, and we find that while for ≲ L * galaxies CGM H i Ly α absorption is stronger as galaxies are more massive, the cool CGM traced by H i Ly α is suppressed above stellar masses of M * ∼ 10 11.5 M ☉ . While most LRG–CGM systems show weak or nondetectable O vi (equivalent width < 0.2 Å), a few LRG–CGM systems show strong O vi 1031, which in most cases likely originates from groups containing both an LRG and a blue star-forming neighboring galaxy.
高晕质量的环星系介质——发光红色星系中冷气体耗竭的特征
摘要研究了15个大质量、淬灭红星系(LRGs)在红移z ~ 0.5、冲击参数高达400kpc的环星系介质(CGM)中的紫外H和金属谱线跃迁。我们选择了8个LRG-CGM系统来研究LRGs周围CGM的一般性质,而其他7个已经从Mg ii光学研究中已知含有冷CGM气体(Mg ii -LRGs)。在一般LRG人群中,我们在8个LRG中检测到4个i,在所有的nh i <病例中;10 16.7 cm−2。相反,所有Mg ii -LRGs均显示H i;对于4个LRGs, H i柱密度为N H i > 10 18 cm−2。LRGs的CGM也显示出低和中等电离谱线(如C iii、C ii、Si iii和Si ii)和O vi的高电离谱线(我们在7个Mg ii -LRGs中检测到5个O vi,在随机样本中检测到8个O vi)。接下来,我们将我们的样本与文献LRGs和> L *星系结合起来,我们发现对于> L *星系,随着星系质量的增加,CGM H i Ly α的吸收更强,而H i Ly α追踪到的冷CGM在恒星质量M * ~ 10 11.5 M☉以上被抑制。虽然大多数LRG-CGM系统显示弱或不可检测的O vi(等效宽度<0.2 Å),一些LRG - cgm系统显示出强烈的O vi 1031,在大多数情况下,它可能来自包含LRG和蓝色恒星形成邻近星系的星系群。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
求助全文
约1分钟内获得全文 求助全文
来源期刊
Astrophysical Journal
Astrophysical Journal 地学天文-天文与天体物理
CiteScore
8.40
自引率
30.60%
发文量
2854
审稿时长
1 months
期刊介绍: The Astrophysical Journal is the foremost research journal in the world devoted to recent developments, discoveries, and theories in astronomy and astrophysics.
×
引用
GB/T 7714-2015
复制
MLA
复制
APA
复制
导出至
BibTeX EndNote RefMan NoteFirst NoteExpress
×
提示
您的信息不完整,为了账户安全,请先补充。
现在去补充
×
提示
您因"违规操作"
具体请查看互助需知
我知道了
×
提示
确定
请完成安全验证×
copy
已复制链接
快去分享给好友吧!
我知道了
右上角分享
点击右上角分享
0
联系我们:info@booksci.cn Book学术提供免费学术资源搜索服务,方便国内外学者检索中英文文献。致力于提供最便捷和优质的服务体验。 Copyright © 2023 布克学术 All rights reserved.
京ICP备2023020795号-1
ghs 京公网安备 11010802042870号
Book学术文献互助
Book学术文献互助群
群 号:481959085
Book学术官方微信