ALMA FIR View of Ultra-high-redshift Galaxy Candidates at z ∼ 11-17: Blue Monsters or Low-z Red Interlopers?

被引：15

作者：

Fujimoto, Seiji ^{[1
,2
,3
]}

Finkelstein, Steven L. ^{[1
]}

Burgarella, Denis ^{[4
]}

Carilli, Chris L. ^{[5
]}

Buat, Veronique ^{[4
]}

Casey, Caitlin M. ^{[1
]}

Ciesla, Laure ^{[4
]}

Tacchella, Sandro ^{[6
,7
]}

Zavala, Jorge A. ^{[8
]}

Brammer, Gabriel ^{[2
,3
]}

Fudamoto, Yoshinobu ^{[9
,10
]}

Ouchi, Masami ^{[8
,11
,12
]}

Valentino, Francesco ^{[2
,3
,13
]}

Cooper, M. C. ^{[14
]}

Dickinson, Mark ^{[15
]}

Franco, Maximilien ^{[1
]}

Giavalisco, Mauro ^{[16
]}

Hutchison, Taylor A. ^{[17
]}

Kartaltepe, Jeyhan S. ^{[18
]}

Koekemoer, Anton M. ^{[19
]}

Kojima, Takashi ^{[11
]}

Larson, Rebecca L. ^{[1
]}

Murphy, E. J. ^{[20
]}

Papovich, Casey ^{[21
,22
]}

Perez-Gonzalez, Pablo G. ^{[23
]}

Somerville, Rachel S. ^{[24
]}

Yoon, Ilsang ^{[20
]}

Wilkins, Stephen M. ^{[25
,26
]}

Akins, Hollis ^{[1
]}

Amorin, Ricardo O. ^{[27
,28
]}

Haro, Pablo Arrabal ^{[15
]}

Bagley, Micaela B. ^{[1
]}

Chworowsky, Katherine ^{[1
]}

Cleri, Nikko J. ^{[21
,22
]}

Cooper, Olivia R. ^{[1
]}

Costantin, Luca ^{[29
]}

Daddi, Emanuele ^{[30
]}

Ferguson, Henry C. ^{[31
]}

Grogin, Norman A. ^{[19
]}

Jimenez-Andrade, E. F. ^{[32
]}

Juneau, Stephanie ^{[33
]}

Kirkpatrick, Allison ^{[34
]}

Kocevski, Dale D. ^{[35
]}

Le Bail, Aurelien ^{[30
]}

Long, Arianna ^{[1
]}

Lucas, Ray A. ^{[19
]}

Magnelli, Benjamin ^{[30
]}

McKinney, Jed ^{[1
]}

Rose, Caitlin ^{[18
]}

Seille, Lise-Marie ^{[4
]}

机构：

[1] Univ Texas Austin, Dept Astron, 2515 Speedway Blvd Stop C1400, Austin, TX 78712 USA

[2] Cosm Dawn Ctr DAWN, Jagtvej 128, DK-2200 Copenhagen N, Denmark

[3] Univ Copenhagen, Niels Bohr Inst, Lyngbyvej 2, DK-2100 Copenhagen O, Denmark

[4] Aix Marseille Univ, CNRS, CNES, LAM Marseille, Marseille, France

[5] Natl Radio Astron Observ, POB O, Socorro, NM 87801 USA

[6] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England

[7] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England

[8] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[9] Waseda Univ, Fac Sci & Engn, Waseda Res Inst Sci & Engn, 3-4-1 Okubo,Shinjuku, Tokyo 1698555, Japan

[10] Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan

[11] Univ Tokyo, Inst Cosm Ray Res, 5-1-5 Kashiwanoha, Kashiwa, Chiba 2778582, Japan

[12] Univ Tokyo, Kavli Inst Phys & Math Universe WPI, Kashiwa, Chiba 2778583, Japan

[13] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[14] Univ Calif Irvine, Dept Phys & Astron, 4129 Reines Hall, Irvine, CA 92697 USA

[15] NSFs Natl Opt Infrared Astron Res Lab, 950 N Cherry Ave, Tucson, AZ 85719 USA

[16] Univ Massachusetts, 710 North Pleasant St, Amherst, MA 01003 USA

[17] NASA, Astrophys Sci Div, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[18] Rochester Inst Technol, Sch Phys & Astron, Lab Multiwavelength Astrophys, 84 Lomb Mem Dr, Rochester, NY 14623 USA

[19] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[20] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA

[21] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[22] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamental, College Stn, TX 77843 USA

[23] Ctr Astrobiol CAB CSIC INTA, Ctra Ajalvir Km 4, E-28850 Madrid, Spain

[24] Flatiron Inst, Ctr Computat Astrophys, 162 5th Ave, New York, NY 10010 USA

[25] Univ Sussex, Astron Ctr, Brighton BN1 9QH, England

[26] Univ Malta, Inst Space Sci & Astron, MSD-2080 Msida, Malta

[27] Univ La Serena, Inst Invest Multidisciplinar Ciencia & Tecnol, Raul Bitran 1305, La Serena 2204000, Chile

[28] Univ La Serena, Dept Astron, Av Juan Cisternas 1200 Norte, La Serena 1720236, Chile

[29] Ctr Astrobiol CSIC INTA, Ctra Ajalvir Km 4, E-28850 Madrid, Spain

[30] Univ Paris Cite, Univ Paris Saclay, CEA, CNRS, F-91191 Gif Sur Yvette, France

[31] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[32] UNAM, Inst Radioastron & Astrofis, Campus Morelia,Apartado Postal 3-72, Morelia 58090, Michoacan, Mexico

[33] NSFs NOIRLab, 950 N Cherry Ave, Tucson, AZ 85719 USA

[34] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA

[35] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA

[36] Univ Arizona, MMT Steward Observ, 933 N Cherry St, Tucson, AZ 85721 USA

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 955卷 / 02期

基金：

新加坡国家研究基金会; 欧洲研究理事会;

关键词：

STELLAR POPULATION SYNTHESIS; DUST-OBSCURED GALAXIES; STAR-FORMING GALAXY; ULTRAVIOLET LUMINOSITY FUNCTIONS; SPECTRAL ENERGY-DISTRIBUTIONS; MASSIVE QUIESCENT GALAXIES; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; SPECTROSCOPIC CONFIRMATION; PHYSICAL-PROPERTIES;

D O I：

10.3847/1538-4357/aceb67

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present Atacama Large Millimeter/submillimeter Array (ALMA) Band 7 observations of a remarkably bright galaxy candidate at (M-UV = -21.6), S5-z17-1, identified in James Webb Space Telescope (JWST) Early Release Observation data of Stephen's Quintet. We do not detect the dust continuum at 866 mu m, ruling out the possibility that S5-z17-1 is a low-z dusty starburst with a star formation rate of greater than or similar to 30 M-circle dot yr(-1). We detect a 5.1s line feature at 338.726 +/- 0.007 GHz exactly coinciding with the JWST source position, with a 2% likelihood of the signal being spurious. The most likely line identification would be [O III]52 mu m at z = 16.01 or [C II]158 mu m at z = 4.61, whose line luminosities do not violate the nondetection of the dust continuum in both cases. Together with three other z greater than or similar to 11-13 candidate galaxies recently observed with ALMA, we conduct a joint ALMA and JWST spectral energy distribution (SED) analysis and find that the high-z solution at z similar to 11-17 is favored in every candidate as a very blue (UV continuum slope of similar or equal to-2.3) and luminous (M-UV similar or equal to [ - 24:-21]) system. Still, we find in several candidates that reasonable SED fits (Delta chi(2) less than or similar to 4) are reproduced by type II quasar and/or quiescent galaxy templates with strong emission lines at z similar to 3-5, where such populations predicted from their luminosity functions and EW([O iii]+H beta) distributions are abundant in survey volumes used for the identification of the z similar to 11-17 candidates. While these recent ALMA observation results have strengthened the likelihood of the high-z solutions, lower-z possibilities are not completely ruled out in several of the z similar to 11-17 candidates, indicating the need to consider the relative surface densities of the lower-z contaminants in the ultra-high-z galaxy search.

引用

页数：21