The Luminosity Function and Star Formation Rate between Redshifts of 0.07 and 1.47 for Narrow-band Emitters in the Subaru Deep Field
Astrophys.J.657:738-759,2007 Abridged: Subaru Deep Field line-emitting galaxies in four narrow-band filters at low and intermediate redshifts are presented. Broad-band colors, follow-up optical spectroscopy, and multiple NB filters are used to distinguish Ha, [O II], and [O III] emitters between red...
Saved in:
Main Authors | , , , , , , , , , |
---|---|
Format | Journal Article |
Language | English |
Published |
27.10.2006
|
Subjects | |
Online Access | Get full text |
Cover
Loading…
Abstract | Astrophys.J.657:738-759,2007 Abridged: Subaru Deep Field line-emitting galaxies in four narrow-band
filters at low and intermediate redshifts are presented. Broad-band colors,
follow-up optical spectroscopy, and multiple NB filters are used to distinguish
Ha, [O II], and [O III] emitters between redshifts of 0.07 and 1.47 to
construct their luminosity functions (LFs). These LFs are derived down to faint
magnitudes, which allows for a more accurate determination of the faint end
slope. With a large (N~200-900) sample for each redshift interval, a Schechter
profile is fitted to each LF. Prior to dust extinction corrections, the [O III]
and [O II] LFs reported in this paper agree reasonably well with those of
Hippelein et al. The z=0.08 Ha LF, which reaches two orders of magnitude
fainter than Gallego et al., is steeper by 25%. This indicates that there are
more low luminosity star-forming galaxies for z<0.1. The faint end slope \alpha
and \phi_{\star} show a strong evolution with redshift while L_{\star} show
little evolution. The evolution in \alpha indicates that low-luminosity
galaxies have a stronger evolution compared to brighter ones. Integrated star
formation rate densities are derived via Ha, [O III], and [O II] for
0.07<z<1.47. A steep increase in the star-formation rate density, as a function
of redshift, is seen for 0.4<z<0.9. For z>1, the star-formation rate densities
are more or less constant. The latter is consistent with previous UV and [O II]
measurements. Below z<0.4, the SFR densities are consistent with several Ha, [O
II], and UV measurements, but other measurements are a factor of two higher.
For example, the z=0.066-0.092 Ha LF agrees with those of Jones &
Bland-Hawthorn, but at z=0.24 and 0.40, their number density is higher by a
factor of two. This discrepancy can be explained by cosmic variance. |
---|---|
AbstractList | Astrophys.J.657:738-759,2007 Abridged: Subaru Deep Field line-emitting galaxies in four narrow-band
filters at low and intermediate redshifts are presented. Broad-band colors,
follow-up optical spectroscopy, and multiple NB filters are used to distinguish
Ha, [O II], and [O III] emitters between redshifts of 0.07 and 1.47 to
construct their luminosity functions (LFs). These LFs are derived down to faint
magnitudes, which allows for a more accurate determination of the faint end
slope. With a large (N~200-900) sample for each redshift interval, a Schechter
profile is fitted to each LF. Prior to dust extinction corrections, the [O III]
and [O II] LFs reported in this paper agree reasonably well with those of
Hippelein et al. The z=0.08 Ha LF, which reaches two orders of magnitude
fainter than Gallego et al., is steeper by 25%. This indicates that there are
more low luminosity star-forming galaxies for z<0.1. The faint end slope \alpha
and \phi_{\star} show a strong evolution with redshift while L_{\star} show
little evolution. The evolution in \alpha indicates that low-luminosity
galaxies have a stronger evolution compared to brighter ones. Integrated star
formation rate densities are derived via Ha, [O III], and [O II] for
0.07<z<1.47. A steep increase in the star-formation rate density, as a function
of redshift, is seen for 0.4<z<0.9. For z>1, the star-formation rate densities
are more or less constant. The latter is consistent with previous UV and [O II]
measurements. Below z<0.4, the SFR densities are consistent with several Ha, [O
II], and UV measurements, but other measurements are a factor of two higher.
For example, the z=0.066-0.092 Ha LF agrees with those of Jones &
Bland-Hawthorn, but at z=0.24 and 0.40, their number density is higher by a
factor of two. This discrepancy can be explained by cosmic variance. |
Author | Kashikawa, Nobunari Malkan, Matt A Shimasaku, Kazuhiro Doi, Mamoru Motohara, Kentaro Iye, Masanori Ly, Chun Nagao, Tohru Morokuma, Tomoki Kodama, Tadayuki |
Author_xml | – sequence: 1 givenname: Chun surname: Ly fullname: Ly, Chun – sequence: 2 givenname: Matt A surname: Malkan fullname: Malkan, Matt A – sequence: 3 givenname: Nobunari surname: Kashikawa fullname: Kashikawa, Nobunari – sequence: 4 givenname: Kazuhiro surname: Shimasaku fullname: Shimasaku, Kazuhiro – sequence: 5 givenname: Mamoru surname: Doi fullname: Doi, Mamoru – sequence: 6 givenname: Tohru surname: Nagao fullname: Nagao, Tohru – sequence: 7 givenname: Masanori surname: Iye fullname: Iye, Masanori – sequence: 8 givenname: Tadayuki surname: Kodama fullname: Kodama, Tadayuki – sequence: 9 givenname: Tomoki surname: Morokuma fullname: Morokuma, Tomoki – sequence: 10 givenname: Kentaro surname: Motohara fullname: Motohara, Kentaro |
BackLink | https://doi.org/10.48550/arXiv.astro-ph/0610846$$DView paper in arXiv https://doi.org/10.1086/510828$$DView published paper (Access to full text may be restricted) |
BookMark | eNqNjr1uwkAQhK8IBQk8A9uktDkL89MHrBQRBdBba7yWV8J31t6an54HD1g8ANVoRjOa79N8OO_ImEli43Q1n9spypXPMQYVH7X11C4Su0oXQ3M_1AR_XcPOB9YbZJ07KnsH6ErYKwpkXhrsox0qQUF6IXoYKkPNlQbwFdjYLvtFEqdLqLzAFkX8JSqe4aZhVZIA7EAfd_uuQOlgTdRCxnQqR2ZQ4SnQ-KVf5jvbHH5-o546b4UblFve0-dtnb_oZ-_2_gH_Kle2 |
ContentType | Journal Article |
DBID | GOX |
DOI | 10.48550/arxiv.astro-ph/0610846 |
DatabaseName | arXiv.org |
DatabaseTitleList | |
Database_xml | – sequence: 1 dbid: GOX name: arXiv.org url: http://arxiv.org/find sourceTypes: Open Access Repository |
DeliveryMethod | fulltext_linktorsrc |
ExternalDocumentID | astro_ph_0610846 |
GroupedDBID | GOX |
ID | FETCH-arxiv_primary_astro_ph_06108463 |
IEDL.DBID | GOX |
IngestDate | Mon Jan 08 05:49:14 EST 2024 |
IsDoiOpenAccess | true |
IsOpenAccess | true |
IsPeerReviewed | false |
IsScholarly | false |
Language | English |
LinkModel | DirectLink |
MergedId | FETCHMERGED-arxiv_primary_astro_ph_06108463 |
OpenAccessLink | https://arxiv.org/abs/astro-ph/0610846 |
ParticipantIDs | arxiv_primary_astro_ph_0610846 |
PublicationCentury | 2000 |
PublicationDate | 2006-10-27 |
PublicationDateYYYYMMDD | 2006-10-27 |
PublicationDate_xml | – month: 10 year: 2006 text: 2006-10-27 day: 27 |
PublicationDecade | 2000 |
PublicationYear | 2006 |
Score | 2.7873795 |
SecondaryResourceType | preprint |
Snippet | Astrophys.J.657:738-759,2007 Abridged: Subaru Deep Field line-emitting galaxies in four narrow-band
filters at low and intermediate redshifts are presented.... |
SourceID | arxiv |
SourceType | Open Access Repository |
SubjectTerms | Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics |
Title | The Luminosity Function and Star Formation Rate between Redshifts of 0.07 and 1.47 for Narrow-band Emitters in the Subaru Deep Field |
URI | https://arxiv.org/abs/astro-ph/0610846 |
hasFullText | 1 |
inHoldings | 1 |
isFullTextHit | |
isPrint | |
link | http://utb.summon.serialssolutions.com/2.0.0/link/0/eLvHCXMwhVxNT4QwEG3cPXkxGjV-buagR3ahW8pyNLq4MbomG024kRZK4LBA-DB694c7LZgYD3qlH6EM7XvTvHmEXOFfksRx4luOSjFBEXrPSR7jdmeSSlcmytHVyE9rvnplD6EbDgJZXQsj6vf8rfcHls1MYLpfWlU2Q9SxESlHZESpFm7dP4e9WMsYcg2jfvdGvmkafgBGsE_2BqYHN31oDsiOKg7JJ4YFHrttXmix1AcECCv60wAm9IDEr4bgu5oQNkgDYdBRwUYlTZanbQNlCvbU9swIZ8o8QNoJa-OlaEn9cLnNjWcm5AUgvQM8G0TdwZ1SFQRasHZEroPly-3KMu8dVb3hRGQWFlVZNCxsfkzGRVmoEwK-UJy7dCE0zrpM-i4VinliHnNuMyZPyeTvuc7-63BOds21A57X1Lsg47bu1CUCcSsnJg5fLimRTQ |
link.rule.ids | 228,230,786,891 |
linkProvider | Cornell University |
openUrl | ctx_ver=Z39.88-2004&ctx_enc=info%3Aofi%2Fenc%3AUTF-8&rfr_id=info%3Asid%2Fsummon.serialssolutions.com&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.atitle=The+Luminosity+Function+and+Star+Formation+Rate+between+Redshifts+of+0.07+and+1.47+for+Narrow-band+Emitters+in+the+Subaru+Deep+Field&rft.au=Ly%2C+Chun&rft.au=Malkan%2C+Matt+A&rft.au=Kashikawa%2C+Nobunari&rft.au=Shimasaku%2C+Kazuhiro&rft.date=2006-10-27&rft_id=info:doi/10.48550%2Farxiv.astro-ph%2F0610846&rft.externalDocID=astro_ph_0610846 |