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Author
dc.contributor.author
Conti, A 
Author
dc.contributor.author
Connolly, A J 
Author
dc.contributor.author
Hopkins, A M 
Author
dc.contributor.author
Budavari, T 
Author
dc.contributor.author
Szalay, A S 
Author
dc.contributor.author
Csabai, I 
Author
dc.contributor.author
Schmidt, S J 
Author
dc.contributor.author
Adams, C 
Author
dc.contributor.author
Petrovic, N 
Availability Date
dc.date.accessioned
2020-08-08T20:18:12Z
Availability Date
dc.date.available
2020-08-08T20:18:12Z
Release
dc.date.issued
2003
uri
dc.identifier.uri
http://hdl.handle.net/10831/49225
Abstract
dc.description.abstract
We analyze the photometric information contained in individual pixels of galaxies in the Hubble Deep Field North (HDF-N) using a new technique, pixel-z, that combines predictions of evolutionary synthesis models with photometric redshift template fitting. Each spectral energy distribution template is a result of modeling of the detailed physical processes affecting gas properties and star formation efficiency. The criteria chosen to generate the spectral energy distribution templates is that of sampling a wide range of physical characteristics such as age, star formation rate, obscuration, and metallicity. A key feature of our method is the sophisticated use of error analysis to generate error maps that de. ne the reliability of the template fitting on pixel scales and allow for the separation of the interplay among dust, metallicity, and star formation histories. This technique offers a number of advantages over traditional integrated color studies. As a first application, we derive the star formation and metallicity histories of galaxies in the HDF-N. Our results show that the comoving density of star formation rate, determined from the UV luminosity density of sources in the HDF-N, increases monotonically with redshift out to at least redshift of 5. This behavior can plausibly be explained by a smooth increase of the UV luminosity density with redshift coupled with an increase in the number of star-forming regions as a function of redshift. We also find that the information contained in individual pixels in a galaxy can be linked to its morphological history. Finally, we derive the metal enrichment rate history of the universe and find it in good agreement with predictions based on the evolving H I content of Lyalpha QSO absorption-line systems.
Language
dc.language
Angol
Title
dc.title
The star formation history of galaxies measured from individual pixels. I. The Hubble Deep Field North
Type
dc.type
folyóiratcikk
Date Change
dc.date.updated
2020-06-05T12:00:22Z
Scope
dc.format.page
2330-2345
Doi ID
dc.identifier.doi
10.1086/378598
Wos ID
dc.identifier.wos
000186494200018
ID Scopus
dc.identifier.scopus
0348199246
MTMT ID
dc.identifier.mtmt
1064344
Issue Number
dc.identifier.issue
5
abbreviated journal
dc.identifier.jabbrev
ASTRON J
Journal
dc.identifier.jtitle
ASTRONOMICAL JOURNAL
Volume Number
dc.identifier.volume
126
Release Date
dc.description.issuedate
2003
department of Author
dc.contributor.institution
Alba Regia Egyetemi Központ
department of Author
dc.contributor.institution
Fizikai Intézet
department of Author
dc.contributor.institution
Mérnöki Intézet
department of Author
dc.contributor.institution
Komplex Rendszerek Fizikája Tanszék
Author institution
dc.contributor.department
Komplex Rendszerek Fizikája Tanszék


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The star formation history of galaxies measured from individual pixels. I. The Hubble Deep Field North
 

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