Three new VHS-DES quasars at 6.7 < z < 6.9 and emission line properties at z > 6.5

被引：82

作者：

Reed, S. L. ^{[1
,2
,3
]}

Banerji, M. ^{[2
,3
]}

Becker, G. D. ^{[4
]}

Hewett, P. C. ^{[2
]}

Martini, P. ^{[5
,6
]}

McMahon, R. G. ^{[2
,3
]}

Pons, E. ^{[2
]}

Rauch, M. ^{[7
]}

Abbott, T. M. C. ^{[8
]}

Allam, S. ^{[9
]}

Annis, J. ^{[9
]}

Avila, S. ^{[10
]}

Bertin, E. ^{[11
,12
]}

Brooks, D. ^{[13
]}

Buckley-Geer, E. ^{[9
]}

Rosell, A. Carnero ^{[14
,15
]}

Kind, M. Carrasco ^{[16
,17
]}

Carretero, J. ^{[18
]}

Castander, F. J. ^{[19
,20
]}

Cunha, C. E. ^{[21
]}

D'Andrea, C. B. ^{[22
]}

da Costa, L. N. ^{[23
]}

De Vicente, J. ^{[14
]}

Desai, S. ^{[24
]}

Diehl, H. T. ^{[9
]}

Doel, P. ^{[13
]}

Evrard, A. E. ^{[25
,26
]}

Flaugher, B. ^{[9
]}

Frieman, J. ^{[9
,15
,27
]}

Garcia-Bellido, J. ^{[28
]}

Gaztanaga, E. ^{[19
,28
]}

Gruen, D. ^{[29
,30
]}

Gschwend, J.

Gutierrez, G.

Hollowood, D. L. ^{[31
]}

Honscheid, K.

Hoyle, B. ^{[32
,33
]}

James, D. J. ^{[34
]}

Kuehn, K. ^{[35
]}

Lahay, O. ^{[13
]}

Lima, M. ^{[15
,36
,37
]}

Maia, M. A. G. ^{[15
]}

Marshall, J. L. ^{[38
,39
]}

Miquel, R. ^{[18
,40
]}

Ogando, R. L. C.

Plazas, A. A. ^{[41
]}

Roodman, A.

Sanchez, E. ^{[14
]}

Scarpine, V. ^{[9
]}

Schubnell, M. ^{[26
]}

机构：

[1] Princeton Univ, Dept Astrophys Sci, 4 Ivy Lane, Princeton, NJ 08544 USA

[2] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

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

[4] Univ Calif Riverside, Dept Phys & Astron, 900 Univ Ave, Riverside, CA 92521 USA

[5] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[6] Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA

[7] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[8] Natl Opt Astron Observ, Cerro Toloto Interamer Observ, Casilla 603, La Serena, Chile

[9] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[10] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England

[11] Inst Astrophys Paris, CNRS, JMR 7095, F-75014 Paris, France

[12] UPMC Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

[13] UCL, Dept Phys & Astron, Gower St, London WC1E 6RT, England

[14] CIEMAT, E-28040 Madrid, Spain

[15] LIneA, Rua Gal Jose Crislino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[16] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[17] Natl Ctr Supercomputing Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[18] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barrelona, Spain

[19] IEEC, E-08034 Barcelona, Spain

[20] CSIC, Inst Space Sci ICE, Carrer Can Magrans,S-N, E-08193 Barcelona, Spain

[21] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA USA

[22] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[23] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[24] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

[25] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[26] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[27] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[28] Univ Autonoma Madrid, Inst Fis Teor UAM CS1C, E-28049 Madrid, Spain

[29] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA

[30] SL4C Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[31] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[32] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

[33] MaX Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[34] Ludwig Maximilian Univ Munchen, Fak Phys, Univ Sternwarte, Scheinetstr 1, D-81679 Munich, Germany

[35] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[36] Macquarie Univ, Australian Astron Opt, Noah Ryde, NSW 2113, Australia

[37] Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil

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

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

[40] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain

[41] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[42] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[43] Univ Estadual Casupinas, Inst Fis Gleb Wataghin, BR-13083859 Campinas, SP, Brazil

[44] Oak Ridge Natl Lab, Comp Sci & Math Divi, Oak Ridge, TN 37831 USA

[45] Argonne Natl Lab, 9700 South Cass Ave, Lemont, IL 60439 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 487卷 / 02期

基金：

英国科学技术设施理事会; 美国国家科学基金会; 欧洲研究理事会;

关键词：

galaxies: active; galaxies: formation; galaxies: high-redshift; dark ages; reionization; first stars; quasars: individual: VDES J0224-4711; quasars: individual: VDES J0244-5008; quasars: individual: VDES J0020-3653; quasars: individual: VDES J0246-5219; TO; 6; QUASARS; BLACK-HOLE; REDSHIFT; WISE; SELECTION; VISTA; WINDS;

D O I：

10.1093/mnras/stz1341

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report the results from a search for z > 6.5 quasars using the Dark Energy Survey (DES) Year 3 data set combined with the VISTA Hemisphere Survey (VHS) and WISE All-Sky Survey. Our photometric selection method is shown to be highly efficient in identifying clean samples of high-redshift quasars, leading to spectroscopic confirmation of three new quasars -VDES J0244-5008 (z = 6,724), VDES J0020-3653 (z = 6.834), and VDES J0246-5219 (z = 6.90) - which were selected as the highest priority candidates in the survey data without any need for additional follow-up observations. We have obtained spectroscopic observations in the near-infrared for VDES J0244-5008 and VDES J0020-3653 as well as our previously identified quasar, VDES J0224-471 1 at z = 6.50 from Reed et al, We use the near-infrared spectra to derive virial black hole masses from the full width at half-maximum of the Mg II line. These black hole masses are similar or equal to 1-2 x 10(9) M-circle dot. Combined with the bolometric luminosities of these quasars of L-bot similar or equal to 1-3 x 10(47), these imply that the Eddington ratios are high, similar or equal to 0.6-1.1. We consider the C iv emission line properties of the sample and demonstrate that our highredshift quasars do not have unusual C iv line properties when compared to carefully matched low-redshift samples. Our new DES + VHS z > 6.5 quasars now add to the growing census of luminous, rapidly accreting supermassive black holes seen well into the epoch of reionization.

引用

页码：1874 / 1885

页数：12

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Three new VHS-DES quasars at 6.7 &lt; z &lt; 6.9 and emission line properties at z &gt; 6.5

Three new VHS-DES quasars at 6.7 < z < 6.9 and emission line properties at z > 6.5