Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26348
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Wang, T. | en_US |
dc.contributor.author | Elbaz, D. | en_US |
dc.contributor.author | Schreiber, C. | en_US |
dc.contributor.author | Pannella, M. | en_US |
dc.contributor.author | Shu, X. | en_US |
dc.contributor.author | Willner, S. P. | en_US |
dc.contributor.author | Ashby, M. L. N. | en_US |
dc.contributor.author | Huang, J. -S. | en_US |
dc.contributor.author | FONTANA, Adriano | en_US |
dc.contributor.author | Dekel, A. | en_US |
dc.contributor.author | Daddi, E. | en_US |
dc.contributor.author | Ferguson, H. C. | en_US |
dc.contributor.author | Dunlop, J. | en_US |
dc.contributor.author | Ciesla, L. | en_US |
dc.contributor.author | Koekemoer, A. M. | en_US |
dc.contributor.author | Giavalisco, M. | en_US |
dc.contributor.author | Boutsia, K. | en_US |
dc.contributor.author | Finkelstein, S. | en_US |
dc.contributor.author | Juneau, S. | en_US |
dc.contributor.author | Barro, G. | en_US |
dc.contributor.author | Koo, D. C. | en_US |
dc.contributor.author | Michałowski, M. J. | en_US |
dc.contributor.author | Orellana, G. | en_US |
dc.contributor.author | Lu, Y. | en_US |
dc.contributor.author | CASTELLANO, MARCO | en_US |
dc.contributor.author | Bourne, N. | en_US |
dc.contributor.author | Buitrago, F. | en_US |
dc.contributor.author | SANTINI, Paola | en_US |
dc.contributor.author | Faber, S. M. | en_US |
dc.contributor.author | Hathi, N. | en_US |
dc.contributor.author | Lucas, R. A. | en_US |
dc.contributor.author | Pérez-González, P. G. | en_US |
dc.date.accessioned | 2020-07-06T18:01:07Z | - |
dc.date.available | 2020-07-06T18:01:07Z | - |
dc.date.issued | 2016 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26348 | - |
dc.description.abstract | We introduce a new color selection technique to identify high-redshift, massive galaxies that are systematically missed by Lyman-break selection. The new selection is based on the H<SUB>160</SUB> (H) and Infrared Array Camera (IRAC) 4.5 μm bands, specifically H-[4.5]\gt 2.25 mag. These galaxies, called “HIEROs,” include two major populations that can be separated with an additional J - H color. The populations are massive and dusty star-forming galaxies at z\gt 3 ({JH}-{blue}) and extremely dusty galaxies at z≲ 3 ({JH}-{red}). The 350 arcmin<SUP>2</SUP> of the GOODS-North and GOODS-South fields with the deepest Hubble Space Telescope (HST)/Wide Field Camera 3 (WFC3) near-infrared and IRAC data contain as many as 285 HIEROs down to [4.5]\lt 24 mag. Inclusion of the most extreme HIEROs, not even detected in the H band, makes this selection particularly complete for the identification of massive high-redshift galaxies. We focus here primarily on {JH}-{blue} (z\gt 3) HIEROs, which have a median photometric redshift < z> ∼ 4.4 and stellar mass {M}<SUB>*</SUB>∼ {10}<SUP>10.6</SUP> {M}<SUB>☉ </SUB> and are much fainter in the rest-frame UV than similarly massive Lyman-break galaxies (LBGs). Their star formation rates (SFRs), derived from their stacked infrared spectral energy distributions (SEDs), reach ∼240 {M}<SUB>☉ </SUB> yr<SUP>-1</SUP>, leading to a specific SFR, {{sSFR}}\equiv {{SFR}}/{M}<SUB>*</SUB>∼ 4.2 Gyr<SUP>-1</SUP>, suggesting that the sSFRs for massive galaxies continue to grow at z\gt 2 but at a lower growth rate than from z = 0 to z = 2. With a median half-light radius of 2 kpc, including ∼ 20% as compact as quiescent (QS) galaxies at similar redshifts, {JH}-{blue} HIEROs represent perfect star-forming progenitors of the most massive ({M}<SUB>*</SUB>≳ {10}<SUP>11.2</SUP> {M}<SUB>☉ </SUB>) compact QS galaxies at z∼ 3 and have the right number density. HIEROs make up ∼ 60% of all galaxies with {M}<SUB>*</SUB>\gt {10}<SUP>10.5</SUP> {M}<SUB>☉ </SUB> identified at z\gt 3 from their photometric redshifts. This is five times more than LBGs with nearly no overlap between the two populations. While HIEROs make up 15%-25% of the total SFR density at z∼ 4-5, they completely dominate the SFR density taking place in {M}<SUB>*</SUB>\gt {10}<SUP>10.5</SUP> {M}<SUB>☉ </SUB> galaxies, and HIEROs are therefore crucial to understanding the very early phase of massive galaxy formation. | en_US |
dc.language.iso | eng | en_US |
dc.title | Infrared Color Selection of Massive Galaxies at z > 3 | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/0004-637X/816/2/84 | en_US |
dc.identifier.scopus | 2-s2.0-84955318949 | en_US |
dc.identifier.isi | 000368238500036 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/0004-637X/816/2/84 | en_US |
dc.identifier.url | https://arxiv.org/abs/1512.02656 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 816 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 84 | en_US |
dc.relation.article | 84 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 32 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | USA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | FRA | en_US |
dc.contributor.country | ESP | en_US |
dc.contributor.country | CHL | en_US |
dc.contributor.country | TWN | en_US |
dc.contributor.country | ISR | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2016ApJ...816...84W | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0004-637X | - |
crisitem.journal.ance | E016252 | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.dept | O.A. Roma | - |
crisitem.author.orcid | 0000-0003-3820-2823 | - |
crisitem.author.orcid | 0000-0001-9875-8263 | - |
crisitem.author.orcid | 0000-0002-9334-8705 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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wang16_open.pdf | postprint | 3.64 MB | Adobe PDF | View/Open |
wang16.pdf | Pdf editoriale | 4 MB | Adobe PDF | View/Open |
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