An Old Stellar Population or Diffuse Nebular Continuum Emission Discovered in Green Pea Galaxies

被引:12
|
作者
Clarke, Leonardo [1 ]
Scarlata, Claudia [1 ]
Mehta, Vihang [1 ]
Keel, William C. [2 ]
Cardamone, Carolin [3 ]
Hayes, Matthew [4 ,5 ]
Adams, Nico [1 ]
Dickinson, Hugh [6 ]
Fortson, Lucy [1 ]
Kruk, Sandor [7 ]
Lintott, Chris [8 ]
Simmons, Brooke [9 ]
机构
[1] Univ Minnesota, Minnesota Inst Astrophys, 116 Church St SE, Minneapolis, MN 55455 USA
[2] Univ Alabama, Dept Phys & Astron, Tuscaloosa, AL 35487 USA
[3] Tufts Univ, 108 Bromfield Rd, Somerville, MA 02144 USA
[4] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden
[5] AlbaNova Univ Ctr, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden
[6] Open Univ, Sch Phys Sci, Milton Keynes MK7 6AA, Bucks, England
[7] European Space Agcy ESA, European Space Res & Technol Ctr ESTEC, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands
[8] Univ Oxford, Dept Phys, Oxford Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England
[9] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England
基金
美国国家航空航天局; 美国国家科学基金会;
关键词
LY-ALPHA; CENT LEAKAGE; EVOLUTION; COMPACT; FRACTION; DUST; I;
D O I
10.3847/2041-8213/abf7cc
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We use new Hubble Space Telescope (HST) images of nine Green Pea galaxies (GPGs) to study their resolved structure and color. The choice of filters, F555W and F850LP, together with the redshift of the galaxies (z similar to 0.25), minimizes the contribution of the nebular [O iii] and H alpha emission lines to the broadband images. While these galaxies are typically very blue in color, our analysis reveals that it is only the dominant stellar clusters that are blue. Each GPG does clearly show the presence of at least one bright and compact star-forming region, but these are invariably superimposed on a more extended and lower surface brightness emission. Moreover, the colors of the star-forming regions are on average bluer than those of the diffuse emission, reaching up to 0.6 magnitudes bluer. Assuming that the diffuse and compact components have constant and single-burst star formation histories, respectively, the observed colors imply that the diffuse components (possibly the host galaxy of the star formation episode) have, on average, old stellar ages (>1 Gyr), while the star clusters are younger than 500 Myr. While a redder stellar component is perhaps the most plausible explanation for these results, the limitations of our current data set lead us to examine possible alternative mechanisms, particularly recombination emission processes, which are unusually prominent in systems with such strong line emission. With the available data, however, it is not possible to distinguish between these two interpretations. A substantial presence of old stars would indicate that the mechanisms allowing large escape fractions in these local galaxies may be different from those at play during the reionization epoch.
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页数:6
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