The JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3
We present an overview and first results from the Spectroscopic Ultradeep Survey Probing Extragalactic Near-infrared Stellar Emission (SUSPENSE), executed with NIRSpec on JWST. The primary goal of the SUSPENSE program is to characterize the stellar, chemical, and kinematic properties of massive quie...
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2024-01-01
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| author | Martje Slob Mariska Kriek Aliza G. Beverage Katherine A. Suess Guillermo Barro Rachel Bezanson Gabriel Brammer Chloe M. Cheng Charlie Conroy Anna de Graaff Natascha M. Förster Schreiber Marijn Franx Brian Lorenz Pavel E. Mancera Piña Danilo Marchesini Adam Muzzin Andrew B. Newman Sedona H. Price Alice E. Shapley Mauro Stefanon Pieter van Dokkum Daniel R. Weisz |
| author_facet | Martje Slob Mariska Kriek Aliza G. Beverage Katherine A. Suess Guillermo Barro Rachel Bezanson Gabriel Brammer Chloe M. Cheng Charlie Conroy Anna de Graaff Natascha M. Förster Schreiber Marijn Franx Brian Lorenz Pavel E. Mancera Piña Danilo Marchesini Adam Muzzin Andrew B. Newman Sedona H. Price Alice E. Shapley Mauro Stefanon Pieter van Dokkum Daniel R. Weisz |
| author_sort | Martje Slob |
| collection | DOAJ |
| description | We present an overview and first results from the Spectroscopic Ultradeep Survey Probing Extragalactic Near-infrared Stellar Emission (SUSPENSE), executed with NIRSpec on JWST. The primary goal of the SUSPENSE program is to characterize the stellar, chemical, and kinematic properties of massive quiescent galaxies at cosmic noon. In a single deep NIRSpec/MSA configuration, we target 20 distant quiescent galaxy candidates ( z = 1–3, H _AB ≤ 23), as well as 53 star-forming galaxies at z = 1–4. With 16 hr of integration and the G140M-F100LP dispersion-filter combination, we observe numerous Balmer and metal absorption lines for all quiescent candidates. We derive stellar masses (log M _* / M _⊙ ∼ 10.2–11.5) and detailed star formation histories (SFHs) and show that all 20 candidate quiescent galaxies indeed have quenched stellar populations. These galaxies show a variety of mass-weighted ages (0.8–3.3 Gyr) and star formation timescales (∼0.5–4 Gyr), and four out of 20 galaxies were already quiescent by z = 3. On average, the z > 1.75 [ z < 1.75] galaxies formed 50% of their stellar mass before z = 4 [ z = 3]. Furthermore, the typical SFHs of the galaxies in these two redshift bins ( z _mean = 2.2 [1.3]) indicate that galaxies at higher redshift formed earlier and over shorter star formation timescales compared to lower redshifts. Although this evolution is naturally explained by the growth of the quiescent galaxy population over cosmic time, number density calculations imply that mergers and/or late-time star formation also contribute to the evolution. In future work, we will further unravel the early formation, quenching, and late-time evolution of these galaxies by extending this work with studies on their chemical abundances, resolved stellar populations, and kinematics. |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
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| spelling | doaj-art-afac22ac63764a2fba0ae83aac39c1722025-01-13T11:30:01ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01973213110.3847/1538-4357/ad65ffThe JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3Martje Slob0https://orcid.org/0000-0001-7540-1544Mariska Kriek1https://orcid.org/0000-0002-7613-9872Aliza G. Beverage2https://orcid.org/0000-0002-9861-4515Katherine A. Suess3https://orcid.org/0000-0002-1714-1905Guillermo Barro4https://orcid.org/0000-0001-6813-875XRachel Bezanson5https://orcid.org/0000-0001-5063-8254Gabriel Brammer6https://orcid.org/0000-0003-2680-005XChloe M. Cheng7https://orcid.org/0000-0003-2251-9164Charlie Conroy8https://orcid.org/0000-0002-1590-8551Anna de Graaff9https://orcid.org/0000-0002-2380-9801Natascha M. Förster Schreiber10https://orcid.org/0000-0003-4264-3381Marijn Franx11https://orcid.org/0000-0002-8871-3026Brian Lorenz12https://orcid.org/0000-0002-5337-5856Pavel E. Mancera Piña13https://orcid.org/0000-0001-5175-939XDanilo Marchesini14https://orcid.org/0000-0001-9002-3502Adam Muzzin15https://orcid.org/0000-0002-9330-9108Andrew B. Newman16https://orcid.org/0000-0001-7769-8660Sedona H. Price17https://orcid.org/0000-0002-0108-4176Alice E. Shapley18https://orcid.org/0000-0003-3509-4855Mauro Stefanon19https://orcid.org/0000-0001-7768-5309Pieter van Dokkum20https://orcid.org/0000-0002-8282-9888Daniel R. Weisz21https://orcid.org/0000-0002-6442-6030Leiden Observatory, Leiden University , P.O. Box 9513, 2300 RA Leiden, The Netherlands ; slob@strw.leidenuniv.nlLeiden Observatory, Leiden University , P.O. Box 9513, 2300 RA Leiden, The Netherlands ; slob@strw.leidenuniv.nlDepartment of Astronomy, University of California , Berkeley, CA 94720, USAKavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University , Stanford, CA 94305, USADepartment of Physics, University of the Pacific , Stockton, CA 90340, USADepartment of Physics and Astronomy and PITT PACC , University of Pittsburgh, Pittsburgh, PA 15260, USACosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK2200 Copenhagen N, DenmarkLeiden Observatory, Leiden University , P.O. Box 9513, 2300 RA Leiden, The Netherlands ; slob@strw.leidenuniv.nlCenter for Astrophysics ∣ Harvard & Smithsonian , Cambridge, MA 02138, USAMax-Planck-Institut für Astronomie , Königstuhl 17, D-69117, Heidelberg, GermanyMax-Planck-Institut für extraterrestrische Physik , Giessenbachstrasse 1, D-85748 Garching, GermanyLeiden Observatory, Leiden University , P.O. Box 9513, 2300 RA Leiden, The Netherlands ; slob@strw.leidenuniv.nlDepartment of Astronomy, University of California , Berkeley, CA 94720, USALeiden Observatory, Leiden University , P.O. Box 9513, 2300 RA Leiden, The Netherlands ; slob@strw.leidenuniv.nlDepartment of Physics & Astronomy, Tufts University , Medford, MA 02155, USADepartment of Physics and Astronomy, York University , 4700 Keele Street, Toronto, ON MJ3 1P3, CanadaObservatories of the Carnegie Institution for Science , 813 Santa Barbara Street, Pasadena, CA 91101, USADepartment of Physics and Astronomy and PITT PACC , University of Pittsburgh, Pittsburgh, PA 15260, USADepartment of Physics & Astronomy, University of California , Los Angeles, CA 90095, USADepartament d’Astronomia i Astrofìsica, Universitat de València , C. Dr. Moliner 50, E-46100 Burjassot, València, Spain; Unidad Asociada CSIC ”Grupo de Astrofísica Extragaláctica y Cosmología” (Instituto de Física de Cantabria - Universitat de València) , SpainAstronomy Department, Yale University , 52 Hillhouse Avenue, New Haven, CT 06511, USADepartment of Astronomy, University of California , Berkeley, CA 94720, USAWe present an overview and first results from the Spectroscopic Ultradeep Survey Probing Extragalactic Near-infrared Stellar Emission (SUSPENSE), executed with NIRSpec on JWST. The primary goal of the SUSPENSE program is to characterize the stellar, chemical, and kinematic properties of massive quiescent galaxies at cosmic noon. In a single deep NIRSpec/MSA configuration, we target 20 distant quiescent galaxy candidates ( z = 1–3, H _AB ≤ 23), as well as 53 star-forming galaxies at z = 1–4. With 16 hr of integration and the G140M-F100LP dispersion-filter combination, we observe numerous Balmer and metal absorption lines for all quiescent candidates. We derive stellar masses (log M _* / M _⊙ ∼ 10.2–11.5) and detailed star formation histories (SFHs) and show that all 20 candidate quiescent galaxies indeed have quenched stellar populations. These galaxies show a variety of mass-weighted ages (0.8–3.3 Gyr) and star formation timescales (∼0.5–4 Gyr), and four out of 20 galaxies were already quiescent by z = 3. On average, the z > 1.75 [ z < 1.75] galaxies formed 50% of their stellar mass before z = 4 [ z = 3]. Furthermore, the typical SFHs of the galaxies in these two redshift bins ( z _mean = 2.2 [1.3]) indicate that galaxies at higher redshift formed earlier and over shorter star formation timescales compared to lower redshifts. Although this evolution is naturally explained by the growth of the quiescent galaxy population over cosmic time, number density calculations imply that mergers and/or late-time star formation also contribute to the evolution. In future work, we will further unravel the early formation, quenching, and late-time evolution of these galaxies by extending this work with studies on their chemical abundances, resolved stellar populations, and kinematics.https://doi.org/10.3847/1538-4357/ad65ffGalaxy evolutionGalaxy quenchingGalaxy formation |
| spellingShingle | Martje Slob Mariska Kriek Aliza G. Beverage Katherine A. Suess Guillermo Barro Rachel Bezanson Gabriel Brammer Chloe M. Cheng Charlie Conroy Anna de Graaff Natascha M. Förster Schreiber Marijn Franx Brian Lorenz Pavel E. Mancera Piña Danilo Marchesini Adam Muzzin Andrew B. Newman Sedona H. Price Alice E. Shapley Mauro Stefanon Pieter van Dokkum Daniel R. Weisz The JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3 The Astrophysical Journal Galaxy evolution Galaxy quenching Galaxy formation |
| title | The JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3 |
| title_full | The JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3 |
| title_fullStr | The JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3 |
| title_full_unstemmed | The JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3 |
| title_short | The JWST-SUSPENSE Ultradeep Spectroscopic Program: Survey Overview and Star Formation Histories of Quiescent Galaxies at 1 < z < 3 |
| title_sort | jwst suspense ultradeep spectroscopic program survey overview and star formation histories of quiescent galaxies at 1 z 3 |
| topic | Galaxy evolution Galaxy quenching Galaxy formation |
| url | https://doi.org/10.3847/1538-4357/ad65ff |
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