The Statistical Properties of Spiral Arms in Nearby Disk Galaxies

被引:28
作者
Yu, Si-Yue [1 ,2 ]
Ho, Luis C. [1 ,2 ]
机构
[1] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China
[2] Peking Univ, Sch Phys, Dept Astron, Beijing 100871, Peoples R China
基金
国家重点研发计划; 美国国家科学基金会;
关键词
Galaxy evolution; Galaxy formation; Spiral galaxies; Hubble classification scheme; Spiral pitch angle; Galaxy structure; DIGITAL SKY SURVEY; GRAND DESIGN; STAR-FORMATION; MORPHOLOGICAL CLASSIFICATIONS; BARRED GALAXIES; STELLAR DISKS; PITCH ANGLES; I; SAMPLE; BARS; DENSITY;
D O I
10.3847/1538-4357/abac5b
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We analyze 4378 nearby bright disk (S0 and spiral) galaxies selected from the Sloan Digital Sky Survey to characterize their spiral structure and systematically investigate the relationships between spiral arm properties (strength, pitch angle, and number) and the global properties of the host galaxies. This is to date the largest sample of galaxies with comprehensive measurements of spiral properties based on Fourier decomposition. We find that spiral pitch angle decreases (arms become more tightly wound) toward galaxies of earlier Hubble type, higher stellar mass, redder color, and greater degree of central concentration. The dependence of pitch angle on stellar mass is mainly driven by color, and for a given concentration, spiral arms are more tightly wound in redder galaxies. Spiral pitch angles show a bimodal distribution, peaking at phi = 12 degrees 34 and 23 degrees 43. Spiral arms weaken in galaxies of earlier type, redder color, and higher concentration, but for a given concentration, spiral arms become more prominent in more massive and bluer galaxies. We confirm that spiral arm strength loosely correlates with pitch angle, although the scatter in this relation is considerable and depends systematically on mass and color; for a given pitch angle, more massive or bluer galaxies have stronger arms. Galaxies of earlier Hubble type, higher mass concentration, or redder color have fewer spiral arms. Lastly, galaxies with stronger bars have fewer but stronger arms. We discuss the possible origins of these various relationships, which provide useful empirical guidance to theories of spiral structure. Depending on the galaxy, both the density wave and swing amplification mechanisms operate.
引用
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页数:18
相关论文
共 96 条
[1]   The population of barred galaxies in the local universe I. Detection and characterisation of bars [J].
Aguerri, J. A. L. ;
Mendez-Abreu, J. ;
Corsini, E. M. .
ASTRONOMY & ASTROPHYSICS, 2009, 495 (02) :491-504
[2]  
Athanassoula E, 2009, MON NOT R ASTRON SOC, V400, P1706, DOI [10.1111/j.1365-2966.2009.15583.x, 10.1111/J.1365-2966.2009.15583.x]
[3]   Galaxy bimodality versus stellar mass and environment [J].
Baldry, I. K. ;
Balogh, M. L. ;
Bower, R. G. ;
Glazebrook, K. ;
Nichol, R. C. ;
Bamford, S. P. ;
Budavari, T. .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2006, 373 (02) :469-483
[4]   Quantifying the bimodal color-magnitude distribution of galaxies [J].
Baldry, IK ;
Glazebrook, K ;
Brinkmann, J ;
Ivezic, Z ;
Lupton, RH ;
Nichol, RC ;
Szalay, AS .
ASTROPHYSICAL JOURNAL, 2004, 600 (02) :681-694
[5]   MODAL APPROACH TO THE MORPHOLOGY OF SPIRAL GALAXIES .1. BASIC STRUCTURE AND ASTROPHYSICAL VIABILITY [J].
BERTIN, G ;
LIN, CC ;
LOWE, SA ;
THURSTANS, RP .
ASTROPHYSICAL JOURNAL, 1989, 338 (01) :78-103
[6]  
Bertin G., 1996, Spiral Structure in Galaxies a Density Wave Theory
[7]  
Binney J., 2008, Galactic Dynamics: Second Edition
[8]   How do spiral arm contrasts relate to bars, disc breaks and other fundamental galaxy properties? [J].
Bittner, Adrian ;
Gadotti, Dimitri A. ;
Elmegreen, Bruce G. ;
Athanassoula, Evangelie ;
Elmegreen, Debra M. ;
Bosma, Albert ;
Munoz-Mateos, Juan-Carlos .
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2017, 471 (01) :1070-1087
[9]   IMPROVED BACKGROUND SUBTRACTION FOR THE SLOAN DIGITAL SKY SURVEY IMAGES [J].
Blanton, Michael R. ;
Kazin, Eyal ;
Muna, Demitri ;
Weaver, Benjamin A. ;
Price-Whelan, Adrian .
ASTRONOMICAL JOURNAL, 2011, 142 (01)
[10]  
Block DL, 1999, ASTRON ASTROPHYS, V342, P627