Published October 27, 2020
| Version v1
Publication
Open
GOODS-ALMA: The slow downfall of star formation in <i>z</i> = 2–3 massive galaxies
Creators
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Maximilien Franco1, 2, 3, 4, 5, 6, 7, 8, 9
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D. Elbaz1, 2, 3, 4, 5, 6, 7, 8
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Luwenjia Zhou2, 3, 4, 5, 6, 7, 8, 10, 1
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B. Magnelli11
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C. Schreiber12
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L. Ciesla13, 14, 6, 1, 2, 3, 4, 5, 7, 8
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Mark Dickinson15, 16
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Neil M. Nagar17
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G. Magdis18, 19, 20
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David Alexander21
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M. Béthermin13, 14, 6
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R. Demarco17
- Emanuele Daddi1, 3, 4, 5, 6, 7, 8, 2
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Ting Wang22, 1, 2, 3, 4, 5, 6, 7, 8
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James Mullaney23
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M. Sargent24
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Hanae Inami25, 26, 27, 6, 28
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Xinwen Shu29
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F. Bournaud2, 3, 4, 5, 6, 7, 8, 1
- Ranga-Ram Chary30, 31
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R. T. Coogan32
- H. C. Ferguson33
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Steven L. Finkelstein34
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Mauro Giavalisco35
- C. Gómez-Guijarro2, 3, 4, 5, 6, 7, 8, 1
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Daisuke Iono36, 37, 38
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Stéphanie Juneau16, 1, 2, 3, 4, 5, 6, 7, 8, 15
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G. Lagache13, 14, 6
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Lihwai Lin39
- Kentaro Motohara22
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K. Okumura3, 4, 5, 6, 7, 8, 1, 2
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M. Pannella40, 41
- C. Papovich42, 43
- Alexandra Pope35
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W. Rujopakarn22, 44, 45, 46
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John D. Silverman46, 22
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Mengyuan Xiao1, 2, 3, 4, 5, 6, 7, 8, 10
- 1. Délégation Paris 7
- 2. Sorbonne Paris Cité
- 3. University of Paris-Saclay
- 4. Université Paris Cité
- 5. Astrophysique, Instrumentation et Modélisation
- 6. Centre National de la Recherche Scientifique
- 7. CEA Saclay
- 8. Atomic Energy and Alternative Energies Commission
- 9. University of Hertfordshire
- 10. Nanjing University
- 11. University of Bonn
- 12. University of Oxford
- 13. Laboratoire d'Astrophysique de Marseille
- 14. Aix-Marseille Université
- 15. Community Science and Data Center
- 16. NSF's NOIRLab
- 17. University of Concepción
- 18. National Observatory of Athens
- 19. University of Copenhagen
- 20. Technical University of Denmark
- 21. Durham University
- 22. The University of Tokyo
- 23. University of Sheffield
- 24. University of Sussex
- 25. Hiroshima University
- 26. Centre de Recherche Astrophysique de Lyon
- 27. Université Claude Bernard Lyon 1
- 28. École Normale Supérieure de Lyon
- 29. Anhui Normal University
- 30. California Institute of Technology
- 31. Infrared Processing and Analysis Center
- 32. Max Planck Institute for Extraterrestrial Physics
- 33. Space Telescope Science Institute
- 34. The University of Texas at Austin
- 35. University of Massachusetts Amherst
- 36. The Graduate University for Advanced Studies, SOKENDAI
- 37. National Astronomical Observatory of Japan
- 38. National Institutes of Natural Sciences
- 39. Institute of Astronomy and Astrophysics, Academia Sinica
- 40. University of Trieste
- 41. Ludwig-Maximilians-Universität München
- 42. Texas A&M University
- 43. Mitchell Institute
- 44. National Astronomical Research Institute of Thailand
- 45. Chulalongkorn University
- 46. Kavli Institute for the Physics and Mathematics of the Universe
Description
We investigate the properties of a sample of 35 galaxies, detected with ALMA at 1.1 mm in the GOODS-ALMA field (area of 69 arcmin$^2$, resolution = 0.60", RMS $\simeq$ 0.18 mJy beam$^{-1}$). Using the UV-to-radio deep multiwavelength coverage of the GOODS-South field, we fit the spectral energy distributions of these galaxies to derive their key physical properties. The galaxies detected by ALMA are among the most massive at $z$ = 2-4 (M$_{\star,med}$ = 8.5$ \times$ 10$^{10}$ M$_\odot$) and are either starburst or located in the upper part of the galaxy star-forming main sequence. A significant portion of our galaxy population ($\sim$ 40%), located at $z\sim$ 2.5-3, exhibits abnormally low gas fractions. The sizes of these galaxies, measured with ALMA, are compatible with the trend between $H$-band size and stellar mass observed for $z\sim2$ elliptical galaxies suggesting that they are building compact bulges. We show that there is a strong link between star formation surface density (at 1.1 mm) and gas depletion time: the more compact a galaxy's star-forming region is, the shorter its lifetime will be (without gas replenishment). The identified compact sources associated with relatively short depletion timescales ($\sim$100 Myr), are the ideal candidates to be the progenitors of compact elliptical galaxies at $z$ $\sim$ 2.
Translated Descriptions
⚠️
This is an automatic machine translation with an accuracy of 90-95%
Translated Description (Arabic)
نقوم بالتحقيق في خصائص عينة من 35 مجرة، تم اكتشافها باستخدام ALMA عند 1.1 مم في حقل GOODS - ALMA (مساحة 69 قوسًا في $^ 2 $، الدقة = 0.60"، RMS $\simeq$ 0.18 mJy beam $^{-1 }$). باستخدام التغطية متعددة الأطوال الموجية العميقة للأشعة فوق البنفسجية إلى الراديو لمجال GOODS - South، نلائم توزيعات الطاقة الطيفية لهذه المجرات لاشتقاق خصائصها الفيزيائية الرئيسية. المجرات التي اكتشفتها ALMA هي من بين الأكثر ضخامة عند $z $= 2-4 (M $_{\star,med }$= 8.5 $\times$ 10 $^{10 }$ M $_\ odot $) وهي إما انفجار نجمي أو تقع في الجزء العلوي من التسلسل الرئيسي لتشكيل نجوم المجرة. يُظهر جزء كبير من سكان مجرتنا ($\ sim$ 40%)، بسعر $ z\sim$ 2.5-3، كسور غاز منخفضة بشكل غير طبيعي. تتوافق أحجام هذه المجرات، التي تم قياسها باستخدام ALMA، مع الاتجاه بين حجم النطاق $H$ والكتلة النجمية التي لوحظت في المجرات البيضاوية $z\ sim2 $ مما يشير إلى أنها تبني انتفاخات مدمجة. نظهر أن هناك صلة قوية بين كثافة سطح تكوين النجوم (عند 1.1 مم) وزمن استنفاد الغاز: كلما كانت منطقة تشكيل النجوم في المجرة أكثر إحكاما، كلما كان عمرها أقصر (بدون تجديد الغاز). المصادر المدمجة المحددة المرتبطة بجداول زمنية قصيرة نسبيًا للنضوب ($\sim$ 100 Myr)، هي المرشحات المثالية لتكون أسلاف المجرات البيضاوية المدمجة بسعر $z $$\ sim$ 2.Translated Description (French)
Nous étudions les propriétés d'un échantillon de 35 galaxies, détecté avec ALMA à 1,1 mm dans le champ GOODS-ALMA (aire de 69 arcmin$^2 $ , résolution = 0,60", faisceau RMS $ \simeq$ 0,18 mJy $^{-1}$ ). En utilisant la couverture UV-radio profonde multi-longueur d'onde du champ GOODS-Sud, nous adaptons les distributions d'énergie spectrale de ces galaxies pour dériver leurs propriétés physiques clés. Les galaxies détectées par ALMA sont parmi les plus massives à $z$ = 2-4 (M$ _ {\star,med}$ = 8,5 $ \times $ 10 $ ^{10} $ M $ _\odot$ ) et sont soit starburst soit situées dans la partie supérieure de la séquence principale de formation d'étoiles de la galaxie. Une partie importante de notre population de galaxies ($ \sim$ 40%), située à $z\sim$ 2,5-3, présente des fractions gazeuses anormalement faibles. Les tailles de ces galaxies, mesurées avec ALMA, sont compatibles avec la tendance entre la taille de la bande $H$ et la masse stellaire observée pour les galaxies elliptiques $z\sim2 $ suggérant qu'elles construisent des renflements compacts. Nous montrons qu'il existe un lien fort entre la densité de surface de la formation stellaire (à 1,1 mm) et le temps d'appauvrissement en gaz : plus la région de formation stellaire d'une galaxie est compacte, plus sa durée de vie sera courte (sans réapprovisionnement en gaz). Les sources compactes identifiées associées à des échelles de temps d'épuisement relativement courtes ($ \sim$ 100 Myr), sont les candidats idéaux pour être les progéniteurs de galaxies elliptiques compactes à $z$ $\sim$ 2.Translated Description (Spanish)
Investigamos las propiedades de una muestra de 35 galaxias, detectadas con ALMA a 1.1 mm en el campo GOODS-ALMA (área de 69 arcmin$^2 $, resolución = 0.60", RMS $\simeq$ 0.18 mJy beam$^{-1}$). Utilizando la cobertura de longitud de onda múltiple profunda de UV a radio del campo GOODS-South, ajustamos las distribuciones de energía espectral de estas galaxias para derivar sus propiedades físicas clave. Las galaxias detectadas por ALMA se encuentran entre las más masivas con $z$ = 2-4 (M$_{\star,med}$ = 8,5 $ \times$ 10 $^{10}$ M$_\odot$) y se encuentran en la parte superior de la secuencia principal de formación estelar de galaxias. Una parte significativa de nuestra población de galaxias ($\sim$ 40%), ubicada en $z\sim$ 2.5-3, exhibe fracciones de gas anormalmente bajas. Los tamaños de estas galaxias, medidos con ALMA, son compatibles con la tendencia entre el tamaño de la banda $H$ y la masa estelar observada para las galaxias elípticas $z\ sim2 $, lo que sugiere que están construyendo protuberancias compactas. Mostramos que existe un fuerte vínculo entre la densidad de la superficie de formación estelar (a 1,1 mm) y el tiempo de agotamiento del gas: cuanto más compacta sea la región de formación estelar de una galaxia, más corta será su vida útil (sin reposición de gas). Las fuentes compactas identificadas asociadas con escalas de tiempo de agotamiento relativamente cortas ($\sim$ 100 Myr), son los candidatos ideales para ser los progenitores de galaxias elípticas compactas a $z$ $\sim$ 2.Files
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Additional details
Additional titles
- Translated title (Arabic)
- GOODS - ALMA: السقوط البطيء لتشكيل النجوم في <i>z</i> = 2–3 مجرات ضخمة
- Translated title (French)
- GOODS-ALMA : La lente chute de la formation d'étoiles dans <i>z</i> = 2–3 galaxies massives
- Translated title (Spanish)
- GOODS-ALMA: La lenta caída de la formación estelar en <i>z</i> = 2–3 galaxias masivas
Identifiers
- Other
- https://openalex.org/W3084182508
- DOI
- 10.1051/0004-6361/202038312
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