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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/31345
DC FieldValueLanguage
dc.contributor.authorBagley, MBen_US
dc.contributor.authorScarlata, Cen_US
dc.contributor.authorMehta, Ven_US
dc.contributor.authorTeplitz, Hen_US
dc.contributor.authorBARONCHELLI, IVANOen_US
dc.contributor.authorEisenstein, DJen_US
dc.contributor.authorPOZZETTI, Luciaen_US
dc.contributor.authorCimatti, Aen_US
dc.contributor.authorRutkowski, Men_US
dc.contributor.authorWang, Yen_US
dc.contributor.authorMerson, Aen_US
dc.date.accessioned2022-01-21T16:10:34Z-
dc.date.available2022-01-21T16:10:34Z-
dc.date.issued2020en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/20.500.12386/31345-
dc.description.abstractThe mutually complementary Euclid and Roman galaxy redshift surveys will use Hα-and [O iii]-selected emission-line galaxies (ELGs) as tracers of the large-scale structure at 0.9 ≲ z ≲ 1.9 (Hα) and 1.5 ≲ z ≲ 2.7 ([O iii]). It is essential to have a reliable and sufficiently precise knowledge of the expected numbers of Hα-emitting galaxies in the survey volume in order to optimize these redshift surveys for the study of dark energy. Additionally, these future samples of ELGs will, like all slitless spectroscopy surveys, be affected by a complex selection function that depends on galaxy size and luminosity, line equivalent width (EW), and redshift errors arising from the misidentification of single ELGs. Focusing on the specifics of the Euclid survey, we combine two slitless spectroscopic WFC3-IR data sets-3D-HST+AGHAST and the WFC3 Infrared Spectroscopic Parallel survey-to construct a Euclid-like sample that covers an area of 0.56 deg2 and includes 1277 ELGs. We detect 1091 (∼3270 deg-2) Hα+[N ii]-emitting galaxies in the range 0.9 ≤ z ≤ 1.6 and 162 (∼440 deg-2) [O iii] λ5007 emitters over 1.5 ≤ z ≤ 2.3 with line fluxes ≥2 × 10-16 erg s-1 cm-2. The median of the Hα+[N ii] EW distribution is ∼250 Å, and the effective radii of the continuum and Hα+[N ii] emission are correlated with a median of ∼0.″38 and significant scatter (σ ∼ 0.″2-0.″35). Finally, we explore the prevalence of redshift misidentification in future Euclid samples, finding potential contamination rates of ∼14%-20% and ∼6% down to 2 × 10-16 erg s-1 cm-2 and 6 × 10-17 erg s-1 cm-2, respectively, although with increased wavelength coverage these percentages drop to nearly zero.en_US
dc.language.isoengen_US
dc.titleHST Grism-derived Forecasts for Future Galaxy Redshift Surveysen_US
dc.typeArticle-
dc.identifier.doi10.3847/1538-4357/ab9828en_US
dc.identifier.scopus2-s2.0-85088051686en_US
dc.identifier.isiWOS:000549305200001en_US
dc.identifier.urlhttps://iopscience.iop.org/article/10.3847/1538-4357/ab9828en_US
dc.identifier.urlhttps://api.elsevier.com/content/abstract/scopus_id/85088051686en_US
dc.relation.mediumSTAMPAen_US
dc.relation.volume897en_US
dc.relation.issue1en_US
dc.relation.firstpage98en_US
dc.type.refereeREF_1en_US
dc.description.internationalsìen_US
dc.relation.scientificsectorFIS/05 - ASTRONOMIA E ASTROFISICAen_US
dc.relation.journalTHE ASTROPHYSICAL JOURNALen_US
dc.type.miur262 Articolo in rivista-
dc.identifier.adsbibcode2020ApJ...897...98Ben_US
dc.description.apcnoen_US
dc.description.oa1 – prodotto con file in versione Open Access (allegare il file al passo  5-Carica)en_US
item.openairetypeArticle-
item.grantfulltextopen-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.languageiso639-1en-
item.cerifentitytypePublications-
item.fulltextWith Fulltext-
crisitem.author.deptIRA Bologna-
crisitem.author.deptOAS Bologna-
crisitem.author.orcid0000-0003-0556-2929-
crisitem.author.orcid0000-0001-7085-0412-
Appears in Collections:1.01 Articoli in rivista
Files in This Item:
File Description SizeFormat
2006.03602.pdfpreprint2.22 MBAdobe PDFView/Open
Bagley_ApJ_2020_1.pdf[Administrators only]3.57 MBAdobe PDF
Bagley_ApJ_2020_2.pdf[Administrators only]270.7 kBAdobe PDF
Bagley_ApJ_2020_3.pdf[Administrators only]257.5 kBAdobe PDF
Bagley_ApJ_2020_4.pdf[Administrators only]4.67 MBAdobe PDF
Bagley_ApJ_2020_5.pdf[Administrators only]6.05 MBAdobe PDF
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