RC100: Rotation Curves of 100 Massive Star-forming Galaxies at z=0.6-2.5 Reveal Little Dark Matter on Galactic Scales

被引:18
作者
Shachar, A. Nestor [1 ]
Price, S. H. [2 ,16 ,17 ]
Schreiber, N. M. Foerster [2 ]
Genzel, R. [2 ,3 ]
Shimizu, T. T. [2 ]
Tacconi, L. J. [2 ]
Ubler, H. [11 ,15 ]
Burkert, A. [4 ]
Davies, R. I. [2 ]
Dekel, A. [6 ]
Herrera-Camus, R. [7 ]
Lee, L. L. [2 ]
Liu, D. [2 ]
Lutz, D. [2 ]
Naab, T. [8 ]
Neri, R. [5 ]
Renzini, A. [9 ]
Saglia, R. [2 ,4 ]
Schuster, K. F. [5 ]
Sternberg, A. [1 ,2 ,10 ]
Wisnioski, E. [12 ,13 ]
Wuyts, S. [14 ]
机构
[1] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel
[2] Max Planck Inst Extraterr Phys MPE, Giessenbachstr 1, D-85748 Garching, Germany
[3] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA
[4] Univ Sternwarte Ludwig Maximilians Univ USM, Scheinerstr 1, D-81679 Munich, Germany
[5] Inst Radioastron Millimetr IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France
[6] Hebrew Univ Jerusalem, Racah Inst Phys, IL-9190401 Jerusalem, Israel
[7] Univ Concepcion, Astron Dept, Ave Esteban Iturra S-N Barrio Univ,Casilla 160, Concepcion, Chile
[8] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany
[9] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy
[10] Flatiron Inst, Ctr Computat Astrophys, 162 5th Ave, New York, NY 10010 USA
[11] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England
[12] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia
[13] ARC Ctr Excellence All Sky Astrophys 3 Dimens ASTR, Sydney, Australia
[14] Univ Bath, Dept Phys, Bath BA2 7AY, England
[15] Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England
[16] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA
[17] Univ Pittsburgh, PITT PACC, Pittsburgh, PA 15260 USA
基金
澳大利亚研究理事会;
关键词
SIMILAR-TO; 2; SINS/ZC-SINF SURVEY; SCALING RELATIONS; QUIESCENT GALAXIES; ANGULAR-MOMENTUM; DRIVEN OUTFLOWS; DENSITY PROFILE; INNER STRUCTURE; GAS KINEMATICS; SURVEY DESIGN;
D O I
10.3847/1538-4357/aca9cf
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We analyze H alpha or CO rotation curves extending out to several galaxy effective radii for 100 massive, large, star-forming disk galaxies (SFGs) across the peak of cosmic galaxy star formation (z similar to 0.6-2.5), more than doubling the previous sample presented by Genzel et al. and Price et al. The observations were taken with SINFONI and KMOS integral-field spectrographs at the ESO-Very Large Telescope, LUCI-LBT, NOEMA-IRAM, and Atacama Large Millimeter/submillimeter Array. We fit the major-axis kinematics with beam-convolved, forward models of turbulent rotating disks with bulges embedded in dark matter (DM) halos, including the effects of pressure support. The fraction of dark to total matter within the disk effective radius (R (e) similar to 5 kpc), f (DM)(R (e)) = V (2) (DM)(R (e))/V (2) (circ)(R (e)) decreases with redshift: at z similar to 1 (z similar to 2) the median DM fraction is 0.38 +/- 0.23 (0.27 +/- 0.18), and a third (half) of all galaxies are maximal disks with f (DM)(R (e)) < 0.28. DM fractions correlate inversely with the baryonic surface density, and the low DM fractions can be explained with a flattened, or cored, inner DM density distribution. At z similar to 2, there is approximate to 40% less DM mass on average within R (e) compared to expected values based on cosmological stellar-mass-halo-mass relations. The DM deficit is more evident at high star formation rate surface densities (greater than or similar to 2.5 M (circle dot) yr(-1) kpc(2)) and galaxies with massive bulges (>= 10(10) M (circle dot)). A combination of stellar or active galactic nucleus feedback, and/or heating due to dynamical friction, may drive the DM from cuspy into cored mass distributions, pointing to an efficient buildup of massive bulges and central black holes at z similar to 2 SFGs.
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页数:25
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