GOALS-JWST: Revealing the Buried Star Clusters in the Luminous Infrared Galaxy VV 114

被引:14
|
作者
Linden, Sean T. [1 ]
Evans, Aaron S. [2 ,3 ]
Armus, Lee [4 ]
Rich, Jeffrey A. [5 ]
Larson, Kirsten L. [6 ]
Lai, Thomas [4 ]
Privon, George C. [7 ]
Vivian, U. [8 ]
Inami, Hanae [9 ]
Bohn, Thomas [9 ]
Song, Yiqing
Barcos-Munoz, Loreto [3 ]
Charmandaris, Vassilis [10 ,11 ,12 ]
Medling, Anne M. [13 ,14 ,15 ]
Stierwalt, Sabrina [16 ]
Diaz-Santos, Tanio
Boker, Torsten [17 ]
van der Werf, Paul [18 ]
Aalto, Susanne [19 ]
Appleton, Philip
Brown, Michael J. I. [20 ]
Hayward, Christopher C. [21 ]
Howell, Justin H. [4 ]
Iwasawa, Kazushi [22 ,23 ]
Kemper, Francisca [24 ,25 ,26 ]
Frayer, David T. [27 ]
Law, David [28 ]
Malkan, Matthew A. [29 ]
Marshall, Jason [30 ]
Mazzarella, Joseph M. [4 ]
Murphy, Eric J. [3 ]
Sanders, David [31 ]
Surace, Jason [4 ]
机构
[1] Univ Massachusetts Amherst, Dept Astron, Amherst, MA 01003 USA
[2] Univ Virginia, Dept Astron, 530 McCormick Rd, Charlottesville, VA 22903 USA
[3] Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA
[4] CALTECH, IPAC, 1200 E Calif Blvd, Pasadena, CA 91125 USA
[5] Observ Carnegie Inst Sci, 813 St Barbara St, Pasadena, CA 91101 USA
[6] AURA European Space Agcy ESA, Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
[7] Univ Florida, Dept Astron, POB 112055, Gainesville, FL 32611 USA
[8] Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA
[9] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, 1-3-1 Kagamiyama, Hiroshima, Hiroshima 7398526, Japan
[10] Univ Crete, Dept Phys, Iraklion 71003, Greece
[11] Fdn Res & Technol Hellas FORTH, Inst Astrophys, Iraklion 70013, Greece
[12] European Univ Cyprus, Sch Sci, Diogenes St, CY-1516 Nicosia, Cyprus
[13] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA
[14] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA
[15] ARC Ctr Excellence All Sky Astrophys 3 Dimens AST, Mt Stromlo, Australia
[16] Occidental Coll, Phys Dept, 1600 Campus Rd, Los Angeles, CA 90042 USA
[17] European Space Agcy, Space Telescope Sci Inst, Baltimore, MD USA
[18] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands
[19] Chalmers Univ Technol, Dept Space Earth & Environm, SE-41296 Gothenburg, Sweden
[20] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia
[21] Flatiron Inst, Ctr Computat Astrophys, 162 Fifth Ave, New York, NY 10010 USA
[22] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti & Franques 1, E-08028 Barcelona, Spain
[23] ICREA, Pg Lluis Co 23, E-08010 Barcelona, Spain
[24] CSIC, Inst Ciencies lEspai ICE, Can Magrans,S-N, E-08193 Barcelona, Spain
[25] ICREA, Pg Lluis Co 23, Barcelona, Spain
[26] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain
[27] Green Bank Observ, 155 Observ Rd, Green Bank, WV 24944 USA
[28] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
[29] UCLA, Dept Phys & Astron, Los Angeles, CA 90095 USA
[30] Glendale Community Coll, 1500 N Verdugo Rd, Glendale, CA 91208 USA
[31] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA
关键词
ANTENNAE GALAXIES; YOUNG; EVOLUTION; DESTRUCTION; POPULATIONS; EMISSION;
D O I
10.3847/2041-8213/acb335
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the results of a James Webb Space Telescope NIRCam investigation into the young massive star cluster (YMC) population in the luminous infrared galaxy VV 114. We identify 374 compact YMC candidates with signal-to-noise ratios >= 3, 5, and 5 at F150W, F200W, and F356W, respectively. A direct comparison with our HST cluster catalog reveals that similar to 20% of these sources are undetected at optical wavelengths. Based on yggdrasil stellar population models, we identify 17 YMC candidates in our JWST imaging alone with F150W - F200W and F200W - F356W colors suggesting they are all very young, dusty (A(V) = 5-15), and massive (10(5.8) < M-circle dot < 10(6.1)). The discovery of these "hidden" sources, many of which are found in the "overlap" region between the two nuclei, quadruples the number of t < 3 Myr clusters and nearly doubles the number of t < 6 Myr clusters detected in VV 114. Now extending the cluster age distribution (dN d tau (sic) t(gamma)) to the youngest ages, we find a slope of gamma = -1.30 +/- 0.39 for 10(6) < tau(yr) < 10(7), which is consistent with the previously determined value from 10(7) < tau(yr) < 10(8.5), and confirms that VV 114 has a steep age distribution slope for all massive star clusters across the entire range of cluster ages observed. Finally, the consistency between our JWST-and HST-derived age distribution slopes indicates that the balance between cluster formation and destruction has not been significantly altered in VV 114 over the last 0.5 Gyr.
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页数:9
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