alx-ai/arxiv_papers · Datasets at Hugging Face

text stringlengths 0 44.4k
SFR(M⊙yr−1) = 1.72×10−10LTIR(L⊙) (4)
In Fig.3, we show the LTIRLFs. Symbols are the same as
Fig.1. Inthe topaxis,we showcorrespondingSFR. Overplott ed
asterisks are cluster LF of MS1054 at z=0.83 with ×2 larger
mass by Bai et al. (2007), which show good agreement with
ourLFsofRXJ1716.4 +6708in thesquares.Notethat Bai et al.
(2007) covered only the central region of MS1054 due to the
smaller ﬁeld of view of the Spitzer. The shape of their LF look s
more similar to our LFs in the highest density bin in Fig.2. A
shift in scale is perhaps due to difference in esimating clus ter
volumes.
Amajordifferenceofourworktothat ofBai etal. (2007)is
that they were not able to compare in detail on the shape of the
LFs between ﬁeld and cluster regions, due mainly to a smaller
ﬁeldcoverageandlargererrorsonLFs.Theyhadtoﬁxthefain t-
end slope with a local value. The largest source of errors is i nGotoet al.:Environemental dependence of 8 µm luminosity functions ofgalaxies atz ∼0.8 5
converting Spitzer 24 µm ﬂux into 8 µm. Both cluster and ﬁeld
LFs of this work use L15ﬁlter, which measures restframe 8 µm
ﬂuxdirectly,eliminatingthelargestsourceoferrors.Ina ddition,
bothclusterandﬁledLFsaremeasuredwithanessentiallysa me
methodology,allowingusa faircomparisonofLFs.
4. Summary
We constructed restframe 8 µm LFs of a massive galaxy cluster
(RXJ1716.4 +6708) and a rareﬁed ﬁeld region (the NEP deep
ﬁeld)at z ∼0.8usingessentially thesame methodanddata from
the AKARI telescope. AKARI’s 15 µm ﬁlter nicely covers rest-
frame8µm at z∼0.8,and thuswe do not needa large interpola-
tion based on SED models. AKARI’s wide ﬁeld of view allows
ustoinvestigatevarietyofclusterenvironmentswith2ord ersof
differenceinlocal galaxydensity.
We found that L∗of the cluster 8 µm LF is smaller than the
ﬁeld by a factor of 2.4, and the faint-end tail of cluster IR LF s
becomesteeperandsteeperwithincreasinglocalgalaxyden sity.
This difference cannot be explained by a simple infall of ﬁel d
galaxies into a cluster. Physics that preferentially supre sses IR
luminous galaxes in higer density regions is needed to expla in
theobservedresults.
Acknowledgments
Wethanktheanonymousrefereeformanyinsightfulcomments ,
which signiﬁcantly improved the paper. We are greateful to
MasayukiTanakaforusefuldiscussion.WethankL.Baiforpr o-
vidingdataforcomparison.
T.G.,Y.K. and H.I. acknowledgesﬁnancial support from the
JapanSocietyforthePromotionofScience(JSPS)throughJS PS
ResearchFellowshipsforYoungScientists.MIwassupporte dby
the Korea Science and Engineering Foundation(KOSEF) grant
No. 2009-0063616, funded by the Korea government(MEST)”
HML acknowledgesthe supportfrom KASI throughits cooper-
ativefundin2008.
This research is based on the observations with AKARI, a
JAXA projectwiththe participationofESA.
Theauthorswishtorecognizeandacknowledgetheverysig-
niﬁcant cultural role and reverence that the summit of Mauna
Kea has always had within the indigenous Hawaiian commu-
nity. We are most fortunate to have the opportunity to conduc t
observationsfromthissacredmountain.
References
Arnouts S.,et al., 2007, A&A,476, 137
Babbedge T.S.R.,et al., 2006, MNRAS,370, 1159
Bai L.,Rieke G.H.,Rieke M. J.,Christlein D.,Zabludoff A.I .,2009, ApJ,693,
1840
Bai L.,Marcillac D.,Rieke G.H.,etal., 2007, ApJ,664, 181
Bai L.,Rieke G.H.,Rieke M.J.,etal., 2006, ApJ,639, 827
Bavouzet N., Dole H., Le Floc’h E., Caputi K. I., Lagache G., K ochanek C. S.,
2008, A&A,479, 83
Brandl B. R.,Bernard-Salas J.,Spoon H.W.W.,et al., 2006, A pJ,653, 1129
Calzetti D.,Kennicutt R.C.,Engelbracht C.W.,etal., 2007 , ApJ,666, 870
Caputi K.I.,etal., 2007, ApJ,660, 97
Dale D.A.,Helou G.,2002, ApJ,576, 159
Desert F.-X.,Boulanger F.,Puget J.L.,1990, A&A,237, 215
Elbaz D.,DaddiE.,LeBorgneD.,et al., 2007, A&A,468, 33
G´ omezP.L.,Nichol R.C., Miller C. J.,et al., 2003, ApJ,584 , 210
Goto, T.,Takagi, T.,Matsuhara, H.,etal., 2010, submitted to A&A
Goto T.,2005, MNRAS,360, 322
Goto T.,Postman M.,Cross N.J.G.,et al.,2005, ApJ, 621,188
Goto T.,Yagi M.,Tanaka M.,Okamura S.,2004, MNRAS,348, 515
Goto T.,Yamauchi C.,Fujita Y.,etal., 2003, MNRAS,346, 601Goto T.,Okamura S.,Sekiguchi M.,etal., 2003, PASJ,55,757
Huang J.-S.,et al.,2007, ApJ, 664,840
Ilbert O.,et al., 2006, A&A,457, 841
ImaiK.,Matsuhara H.,Oyabu S.et al., 2007, AJ,133,2418
Kennicutt R.C.,Jr., 1998, ARA&A,36,189
Kodama T., Balogh M. L., Smail I., Bower R. G., Nakata F., 2004 , MNRAS,
354, 1103
Komatsu E.,Dunkley J.,Nolta M.R.,et al.,2009, ApJS, 180,3 30
Koyama Y.,KodamaT.,Shimasaku K.,et al., 2008, MNRAS,391, 1758
KoyamaY.,KodamaT.,TanakaM.,Shimasaku K.,OkamuraS.,20 07,MNRAS,
382, 1719
Lagache G.,Dole H.,Puget J.-L.,2003, MNRAS, 338, 555
Matsuhara H.,etal., 2007, PASJ,59,543
Matsuhara H.,etal., 2006, PASJ,58,673
Murakami H.,et al.,2007, PASJ,59, 369
Pearson C.,et al. 2009, A&A,submitted
Rieke G.H.,Alonso-Herrero A.,Weiner B. J.,etal., 2009, Ap J,692, 556
Shim H.,etal. 2010, ApJ, submitted
Sutherland W.,Saunders W.,1992, MNRAS, 259, 413
Takeuchi T.T.,Buat V.,Burgarella D.,2005, A&A,440, L17
Tanaka M.,Finoguenov A.,Kodama T.,et al.,2008, A&A,489, 5 71
Tanaka M.,KodamaT.,Arimoto N.,etal., 2005, MNRAS, 362,26 8
Tanaka M., Goto T., Okamura S., Shimasaku K., Brinkmann J., 2 004, AJ, 128,
2677

SFR(M⊙yr−1) = 1.72×10−10LTIR(L⊙) (4)

In Fig.3, we show the LTIRLFs. Symbols are the same as

Fig.1. Inthe topaxis,we showcorrespondingSFR. Overplott ed

asterisks are cluster LF of MS1054 at z=0.83 with ×2 larger

mass by Bai et al. (2007), which show good agreement with

ourLFsofRXJ1716.4 +6708in thesquares.Notethat Bai et al.

(2007) covered only the central region of MS1054 due to the

smaller ﬁeld of view of the Spitzer. The shape of their LF look s

more similar to our LFs in the highest density bin in Fig.2. A

shift in scale is perhaps due to difference in esimating clus ter

volumes.

Amajordifferenceofourworktothat ofBai etal. (2007)is

that they were not able to compare in detail on the shape of the

LFs between ﬁeld and cluster regions, due mainly to a smaller

ﬁeldcoverageandlargererrorsonLFs.Theyhadtoﬁxthefain t-

end slope with a local value. The largest source of errors is i nGotoet al.:Environemental dependence of 8 µm luminosity functions ofgalaxies atz ∼0.8 5

converting Spitzer 24 µm ﬂux into 8 µm. Both cluster and ﬁeld

LFs of this work use L15ﬁlter, which measures restframe 8 µm

ﬂuxdirectly,eliminatingthelargestsourceoferrors.Ina ddition,

bothclusterandﬁledLFsaremeasuredwithanessentiallysa me

methodology,allowingusa faircomparisonofLFs.

4. Summary

We constructed restframe 8 µm LFs of a massive galaxy cluster

(RXJ1716.4 +6708) and a rareﬁed ﬁeld region (the NEP deep

ﬁeld)at z ∼0.8usingessentially thesame methodanddata from

the AKARI telescope. AKARI’s 15 µm ﬁlter nicely covers rest-

frame8µm at z∼0.8,and thuswe do not needa large interpola-

tion based on SED models. AKARI’s wide ﬁeld of view allows

ustoinvestigatevarietyofclusterenvironmentswith2ord ersof

differenceinlocal galaxydensity.

We found that L∗of the cluster 8 µm LF is smaller than the

ﬁeld by a factor of 2.4, and the faint-end tail of cluster IR LF s

becomesteeperandsteeperwithincreasinglocalgalaxyden sity.

This difference cannot be explained by a simple infall of ﬁel d

galaxies into a cluster. Physics that preferentially supre sses IR

luminous galaxes in higer density regions is needed to expla in

theobservedresults.

Acknowledgments

Wethanktheanonymousrefereeformanyinsightfulcomments ,

which signiﬁcantly improved the paper. We are greateful to

MasayukiTanakaforusefuldiscussion.WethankL.Baiforpr o-

vidingdataforcomparison.

T.G.,Y.K. and H.I. acknowledgesﬁnancial support from the

JapanSocietyforthePromotionofScience(JSPS)throughJS PS

ResearchFellowshipsforYoungScientists.MIwassupporte dby

the Korea Science and Engineering Foundation(KOSEF) grant

No. 2009-0063616, funded by the Korea government(MEST)”

HML acknowledgesthe supportfrom KASI throughits cooper-

ativefundin2008.

This research is based on the observations with AKARI, a

JAXA projectwiththe participationofESA.

Theauthorswishtorecognizeandacknowledgetheverysig-

niﬁcant cultural role and reverence that the summit of Mauna

Kea has always had within the indigenous Hawaiian commu-

nity. We are most fortunate to have the opportunity to conduc t

observationsfromthissacredmountain.

References

Arnouts S.,et al., 2007, A&A,476, 137

Babbedge T.S.R.,et al., 2006, MNRAS,370, 1159

Bai L.,Rieke G.H.,Rieke M. J.,Christlein D.,Zabludoff A.I .,2009, ApJ,693,

1840

Bai L.,Marcillac D.,Rieke G.H.,etal., 2007, ApJ,664, 181

Bai L.,Rieke G.H.,Rieke M.J.,etal., 2006, ApJ,639, 827

Bavouzet N., Dole H., Le Floc’h E., Caputi K. I., Lagache G., K ochanek C. S.,

2008, A&A,479, 83

Brandl B. R.,Bernard-Salas J.,Spoon H.W.W.,et al., 2006, A pJ,653, 1129

Calzetti D.,Kennicutt R.C.,Engelbracht C.W.,etal., 2007 , ApJ,666, 870

Caputi K.I.,etal., 2007, ApJ,660, 97

Dale D.A.,Helou G.,2002, ApJ,576, 159

Desert F.-X.,Boulanger F.,Puget J.L.,1990, A&A,237, 215

Elbaz D.,DaddiE.,LeBorgneD.,et al., 2007, A&A,468, 33

G´ omezP.L.,Nichol R.C., Miller C. J.,et al., 2003, ApJ,584 , 210

Goto, T.,Takagi, T.,Matsuhara, H.,etal., 2010, submitted to A&A

Goto T.,2005, MNRAS,360, 322

Goto T.,Postman M.,Cross N.J.G.,et al.,2005, ApJ, 621,188

Goto T.,Yagi M.,Tanaka M.,Okamura S.,2004, MNRAS,348, 515

Goto T.,Yamauchi C.,Fujita Y.,etal., 2003, MNRAS,346, 601Goto T.,Okamura S.,Sekiguchi M.,etal., 2003, PASJ,55,757

Huang J.-S.,et al.,2007, ApJ, 664,840

Ilbert O.,et al., 2006, A&A,457, 841

ImaiK.,Matsuhara H.,Oyabu S.et al., 2007, AJ,133,2418

Kennicutt R.C.,Jr., 1998, ARA&A,36,189

Kodama T., Balogh M. L., Smail I., Bower R. G., Nakata F., 2004 , MNRAS,

354, 1103

Komatsu E.,Dunkley J.,Nolta M.R.,et al.,2009, ApJS, 180,3 30

Koyama Y.,KodamaT.,Shimasaku K.,et al., 2008, MNRAS,391, 1758

KoyamaY.,KodamaT.,TanakaM.,Shimasaku K.,OkamuraS.,20 07,MNRAS,

382, 1719

Lagache G.,Dole H.,Puget J.-L.,2003, MNRAS, 338, 555

Matsuhara H.,etal., 2007, PASJ,59,543

Matsuhara H.,etal., 2006, PASJ,58,673

Murakami H.,et al.,2007, PASJ,59, 369

Pearson C.,et al. 2009, A&A,submitted

Rieke G.H.,Alonso-Herrero A.,Weiner B. J.,etal., 2009, Ap J,692, 556

Shim H.,etal. 2010, ApJ, submitted

Sutherland W.,Saunders W.,1992, MNRAS, 259, 413

Takeuchi T.T.,Buat V.,Burgarella D.,2005, A&A,440, L17

Tanaka M.,Finoguenov A.,Kodama T.,et al.,2008, A&A,489, 5 71

Tanaka M.,KodamaT.,Arimoto N.,etal., 2005, MNRAS, 362,26 8

Tanaka M., Goto T., Okamura S., Shimasaku K., Brinkmann J., 2 004, AJ, 128,

2677