alx-ai/arxiv_papers · Datasets at Hugging Face

text stringlengths 0 44.4k
5.8(1.4) 4 .49(97)×10−31621(173)
8.0(2.9) 4 .75(46)×10−31480(82)
TrES-4b152250(37) 3.6(0.75) 1 .37(11)×10−31889(63) Td=1891(81) K
4.5(1.0) 1 .48(16)×10−31727(83)
5.8(1.4) 2 .61(59)×10−32112(283)
8.0(2.9) 3 .18(44)×10−32168(197)
WASP-1b162347(35) 3.6(0.75) 1 .17(16)×10−31678(87) Td=1719(89) K
4.5(1.0) 2 .12(21)×10−31923(91)
5.8(1.4) 2 .82(60)×10−32042(253)
8.0(2.9) 4 .70(46)×10−32587(176)
WASP-2b171661(69) 3.6(0.75) 8 .3(3.5)×10−41264(164) Td=1280(121) K
4.5(1.0) 1 .69(17)×10−31380(53)
5.8(1.4) 1 .92(77)×10−31299(232)
8.0(2.9) 2 .85(59)×10−31372(154)
WASP-4b182163(60) 3.6(0.75) 3 .19(31)×10−32156(97) Td=2146(140) K
4.5(1.0) 3 .43(27)×10−31971(75)
WASP-12b193213(119) 0.9(0.15) 8 .2(1.5)×10−43002(104) Td=2939(98) K
1.25(0.16) 1 .31(28)×10−32894(149)
1.65(0.25) 1 .76(18)×10−32823(88)
2.15(0.32) 3 .09(13)×10−33018(51)
3.6(0.75) 3 .79(13)×10−32704(49)
4.5(1.0) 3 .82(19)×10−32486(68)
5.8(1.4) 6 .29(52)×10−33167(179)
8.0(2.9) 6 .36(67)×10−32996(229)
WASP-18b203070(50) 3.6(0.75) 3 .1(2)×10−33000(107) Td=2998(138) K
4.5(1.0) 3 .8(3)×10−33128(150)
5.8(1.4) 4 .1(2)×10−33095(103)
8.0(2.9) 4 .3(3)×10−32991(153)
WASP-19b212581(49) 1.65(0.25) 2 .59(45)×10−32677(135) Td=2677(244) K
XO-1b221526(24) 3.6(0.75) 8 .6(7)×10−41300(32) Td=1306(47) K
4.5(1.0) 1 .22(9)×10−31265(34)
5.8(1.4) 2 .61(31)×10−31546(89)
8.0(2.9) 2 .10(29)×10−31211(87)
XO-2231685(33) 3.6(0.75) 8 .1(1.7)×10−41447(102) Td=1431(98) K
4.5(1.0) 9 .8(2.0)×10−41341(105)
5.8(1.4) 1 .67(36)×10−31497(155)
8.0(2.9) 1 .33(49)×10−31179(219)
XO-3241982(82) 3.6(0.75) 1 .01(4)×10−31875(30) Td=1871(63) K
4.5(1.0) 1 .43(6)×10−31965(40)
5.8(1.4) 1 .34(49)×10−31716(330)
8.0(2.9) 1 .50(36)×10−31625(236)
aThe planet’s expected day-side eﬀective temperature in the absence of reﬂection or recirculation ( AB= 0,ε= 0). The 1 σuncertainty is shown
in parenthese.
bThe bandwidth is shown in parenthese.
cEclipse depths and phase amplitudes are unitless, since the y are measured relative to stellar ﬂux.
dTdandTndenote the day-side and night-side eﬀective temperatures o f the planet, as estimated from thermal secondary eclipse de pths and
thermal phase variations, respectively. The estimated 1 σuncertainties are shown in parentheses. The default day-si de temperature is computed
using only observations at λ >0.8µm. Eclipse measurements at shorter wavelengths may then be u sed to estimate the planet’s albedo at those
wavelengths, Aλ. Note that this is a spherical albedo; the geometric albedo i s given by Ag=2
3Aλ. If —on the other hand— AB= 0 is assumed,
then all the day-side ﬂux is thermal, regardless of waveband , yielding the second Tdestimate.
eWhen multiple measurements of an eclipse depth have been pub lished in a given waveband, we use the most recent observatio n. In all cases
these observations are either explicitly agree with their o lder counterpart, or agree with the re-analyzed older data.
1Snellen et al. (2009); Alonso et al. (2009b); Gillon et al. (2 009); Rogers et al. (2009); Deming et al. (2010),2Alonso et al. (2009a); Snellen et al.
(2010); Gillon et al. (2010); Alonso et al. (2010); Deming et al. (2010),3Deming et al. (2007); Demory et al. (2007); Stevenson et al. ( 2010);
Knutson et al. in prep.,4Todorov et al. (2010),5Borucki et al. (2009); Christiansen et al. (2010),6Laughlin et al. (2009),7Knutson et al.
(2009b),8Deming et al. (2006); Knutson et al. (2007a); Barnes et al. (2 007); Charbonneau et al. (2008); Knutson et al. (2009c); Ago l et al.
(2010),9Richardson et al. (2003); Deming et al. (2005); Cowan et al. ( 2007); Rowe et al. (2008); Knutson et al. (2008),10Sing & L´ opez-Morales
(2009),11Snellen & Covino (2007),12Charbonneau et al. (2005); Knutson et al. (2007b),13O’Donovan et al. (2010); Croll et al. (2010a);
Kipping & Bakos (2010b),14Fressin et al. (2010); Croll et al. (2010b); Christiansen et al. (2010b),15Knutson et al. (2009a),16,17Wheatley et al.
(2010),18Beerer et al. (2010),19L´ opez-Morales et al. (2010); Campo et al. (2010); Croll et a l. (2010c),20Nymeyer et al. (2010),21Anderson et al.
(2010),22Machalek et al. (2008),23Machalek et al. (2009),24Machalek et al. (2010)
arXiv:1001.0013v2 [astro-ph.CO] 8 Jan 2010Astronomy& Astrophysics manuscriptno.akari˙LF˙aa˙v7 c∝circlecopyrtESO 2018
October30,2018
EvolutionofInfraredLuminosityfunctionsofGalaxiesint he
AKARINEP-Deepﬁeld
Revealing thecosmic star formationhistory hidden by dust⋆,⋆⋆
Tomotsugu Goto1,2,⋆⋆⋆,T.Takagi3,H.Matsuhara3,T.T.Takeuchi4,C.Pearson5,6,7, T.Wada3,T.Nakagawa3,O.Ilbert8,
E.LeFloc’h9,S.Oyabu3, Y.Ohyama10,M.Malkan11, H.M.Lee12, M.G.Lee12,H.Inami3,13,14, N.Hwang2, H.Hanami15,
M.Im12, K.Imai16,T.Ishigaki17,S.Serjeant7,and H.Shim12
1Institute for Astronomy, University of Hawaii,2680 Woodla wnDrive, Honolulu, HI,96822, USA
e-mail:tomo@ifa.hawaii.edu
2National Astronomical Observatory, 2-21-1 Osawa,Mitaka, Tokyo, 181-8588,Japan
3Institute of Space and Astronautical Science, JapanAerosp ace Exploration Agency, Sagamihara,Kanagawa 229-8510
4Institute for Advanced Research, Nagoya University, Furo- cho, Chikusa-ku, Nagoya 464-8601
5Rutherford Appleton Laboratory, Chilton, Didcot,Oxfords hire OX110QX, UK
6Department of Physics,Universityof Lethbridge, 4401 Univ ersity Drive,Lethbridge, AlbertaT1J 1B1, Canada
7Astrophysics Group, Department of Physics, The OpenUniver sity, MiltonKeynes, MK76AA, UK
8Laboratoire d’Astrophysique de Marseille, BP8,Traverse d u Siphon, 13376 Marseille Cedex 12, France
9CEA-Saclay,Service d’Astrophysique, France
10Academia Sinica,Institute of Astronomyand Astrophysics, Taiwan
11Department of Physicsand Astronomy, UCLA,Los Angeles, CA, 90095-1547 USA
12Department of Physics& Astronomy, FPRD,Seoul National Uni versity, Shillim-Dong,Kwanak-Gu, Seoul 151-742, Korea
13Spitzer Science Center,California Institute ofTechnolog y, Pasadena, CA91125
14Department of Astronomical Science,The Graduate Universi tyfor Advanced Studies
15Physics Section,Facultyof Humanities and SocialSciences , Iwate University, Morioka, 020-8550
16TOMER&D Inc. Kawasaki, Kanagawa 2130012, Japan
17Asahikawa National College of Technology, 2-1-6 2-joShunk ohdai, Asahikawa-shi, Hokkaido 071-8142
Received September 15, 2009; accepted December 16, 2009
ABSTRACT
Aims.Dust-obscured star-formation becomes much more important with increasing intensity, and increasing redshift. We aim to
reveal cosmic star-formationhistoryobscured bydust usin g deep infraredobservation withthe AKARI.
Methods. We construct restframe 8 µm, 12µm, and total infrared (TIR) luminosity functions (LFs) at 0.15< z <2.2using 4128
infraredsources intheAKARINEP-Deepﬁeld.Acontinuous ﬁl tercoverage inthemid-IRwavelength(2.4,3.2,4.1,7,9,11 , 15,18,
and 24µm) by the AKARI satellite allows us to estimate restframe 8 µm and 12 µm luminosities without using a large extrapolation
based ona SEDﬁt,which was the largestuncertainty inprevio us work.
Results. Wehavefoundthatall8 µm(0.38< z <2.2),12µm(0.15< z <1.16),andTIRLFs( 0.2< z <1.6),showacontinuous
andstrongevolutiontowardhigher redshift.Intermsofcos micinfraredluminositydensity( ΩIR),whichwasobtainedbyintegrating
analytic ﬁts to the LFs,we found a good agreement withprevio us work at z <1.2. We found the ΩIRevolves as ∝(1+z)4.4±1.0.
Whenweseparatecontributionsto ΩIRbyLIRGsandULIRGs,wefoundmoreIRluminoussourcesareinc reasinglymoreimportant

5.8(1.4) 4 .49(97)×10−31621(173)

8.0(2.9) 4 .75(46)×10−31480(82)

TrES-4b152250(37) 3.6(0.75) 1 .37(11)×10−31889(63) Td=1891(81) K

4.5(1.0) 1 .48(16)×10−31727(83)

5.8(1.4) 2 .61(59)×10−32112(283)

8.0(2.9) 3 .18(44)×10−32168(197)

WASP-1b162347(35) 3.6(0.75) 1 .17(16)×10−31678(87) Td=1719(89) K

4.5(1.0) 2 .12(21)×10−31923(91)

5.8(1.4) 2 .82(60)×10−32042(253)

8.0(2.9) 4 .70(46)×10−32587(176)

WASP-2b171661(69) 3.6(0.75) 8 .3(3.5)×10−41264(164) Td=1280(121) K

4.5(1.0) 1 .69(17)×10−31380(53)

5.8(1.4) 1 .92(77)×10−31299(232)

8.0(2.9) 2 .85(59)×10−31372(154)

WASP-4b182163(60) 3.6(0.75) 3 .19(31)×10−32156(97) Td=2146(140) K

4.5(1.0) 3 .43(27)×10−31971(75)

WASP-12b193213(119) 0.9(0.15) 8 .2(1.5)×10−43002(104) Td=2939(98) K

1.25(0.16) 1 .31(28)×10−32894(149)

1.65(0.25) 1 .76(18)×10−32823(88)

2.15(0.32) 3 .09(13)×10−33018(51)

3.6(0.75) 3 .79(13)×10−32704(49)

4.5(1.0) 3 .82(19)×10−32486(68)

5.8(1.4) 6 .29(52)×10−33167(179)

8.0(2.9) 6 .36(67)×10−32996(229)

WASP-18b203070(50) 3.6(0.75) 3 .1(2)×10−33000(107) Td=2998(138) K

4.5(1.0) 3 .8(3)×10−33128(150)

5.8(1.4) 4 .1(2)×10−33095(103)

8.0(2.9) 4 .3(3)×10−32991(153)

WASP-19b212581(49) 1.65(0.25) 2 .59(45)×10−32677(135) Td=2677(244) K

XO-1b221526(24) 3.6(0.75) 8 .6(7)×10−41300(32) Td=1306(47) K

4.5(1.0) 1 .22(9)×10−31265(34)

5.8(1.4) 2 .61(31)×10−31546(89)

8.0(2.9) 2 .10(29)×10−31211(87)

XO-2231685(33) 3.6(0.75) 8 .1(1.7)×10−41447(102) Td=1431(98) K

4.5(1.0) 9 .8(2.0)×10−41341(105)

5.8(1.4) 1 .67(36)×10−31497(155)

8.0(2.9) 1 .33(49)×10−31179(219)

XO-3241982(82) 3.6(0.75) 1 .01(4)×10−31875(30) Td=1871(63) K

4.5(1.0) 1 .43(6)×10−31965(40)

5.8(1.4) 1 .34(49)×10−31716(330)

8.0(2.9) 1 .50(36)×10−31625(236)

aThe planet’s expected day-side eﬀective temperature in the absence of reﬂection or recirculation ( AB= 0,ε= 0). The 1 σuncertainty is shown

in parenthese.

bThe bandwidth is shown in parenthese.

cEclipse depths and phase amplitudes are unitless, since the y are measured relative to stellar ﬂux.

dTdandTndenote the day-side and night-side eﬀective temperatures o f the planet, as estimated from thermal secondary eclipse de pths and

thermal phase variations, respectively. The estimated 1 σuncertainties are shown in parentheses. The default day-si de temperature is computed

using only observations at λ >0.8µm. Eclipse measurements at shorter wavelengths may then be u sed to estimate the planet’s albedo at those

wavelengths, Aλ. Note that this is a spherical albedo; the geometric albedo i s given by Ag=2

3Aλ. If —on the other hand— AB= 0 is assumed,

then all the day-side ﬂux is thermal, regardless of waveband , yielding the second Tdestimate.

eWhen multiple measurements of an eclipse depth have been pub lished in a given waveband, we use the most recent observatio n. In all cases

these observations are either explicitly agree with their o lder counterpart, or agree with the re-analyzed older data.

1Snellen et al. (2009); Alonso et al. (2009b); Gillon et al. (2 009); Rogers et al. (2009); Deming et al. (2010),2Alonso et al. (2009a); Snellen et al.

(2010); Gillon et al. (2010); Alonso et al. (2010); Deming et al. (2010),3Deming et al. (2007); Demory et al. (2007); Stevenson et al. ( 2010);

Knutson et al. in prep.,4Todorov et al. (2010),5Borucki et al. (2009); Christiansen et al. (2010),6Laughlin et al. (2009),7Knutson et al.

(2009b),8Deming et al. (2006); Knutson et al. (2007a); Barnes et al. (2 007); Charbonneau et al. (2008); Knutson et al. (2009c); Ago l et al.

(2010),9Richardson et al. (2003); Deming et al. (2005); Cowan et al. ( 2007); Rowe et al. (2008); Knutson et al. (2008),10Sing & L´ opez-Morales

(2009),11Snellen & Covino (2007),12Charbonneau et al. (2005); Knutson et al. (2007b),13O’Donovan et al. (2010); Croll et al. (2010a);

Kipping & Bakos (2010b),14Fressin et al. (2010); Croll et al. (2010b); Christiansen et al. (2010b),15Knutson et al. (2009a),16,17Wheatley et al.

(2010),18Beerer et al. (2010),19L´ opez-Morales et al. (2010); Campo et al. (2010); Croll et a l. (2010c),20Nymeyer et al. (2010),21Anderson et al.

(2010),22Machalek et al. (2008),23Machalek et al. (2009),24Machalek et al. (2010)

arXiv:1001.0013v2 [astro-ph.CO] 8 Jan 2010Astronomy& Astrophysics manuscriptno.akari˙LF˙aa˙v7 c∝circlecopyrtESO 2018

October30,2018

EvolutionofInfraredLuminosityfunctionsofGalaxiesint he

AKARINEP-Deepﬁeld

Revealing thecosmic star formationhistory hidden by dust⋆,⋆⋆

Tomotsugu Goto1,2,⋆⋆⋆,T.Takagi3,H.Matsuhara3,T.T.Takeuchi4,C.Pearson5,6,7, T.Wada3,T.Nakagawa3,O.Ilbert8,

E.LeFloc’h9,S.Oyabu3, Y.Ohyama10,M.Malkan11, H.M.Lee12, M.G.Lee12,H.Inami3,13,14, N.Hwang2, H.Hanami15,

M.Im12, K.Imai16,T.Ishigaki17,S.Serjeant7,and H.Shim12

1Institute for Astronomy, University of Hawaii,2680 Woodla wnDrive, Honolulu, HI,96822, USA

e-mail:tomo@ifa.hawaii.edu

2National Astronomical Observatory, 2-21-1 Osawa,Mitaka, Tokyo, 181-8588,Japan

3Institute of Space and Astronautical Science, JapanAerosp ace Exploration Agency, Sagamihara,Kanagawa 229-8510

4Institute for Advanced Research, Nagoya University, Furo- cho, Chikusa-ku, Nagoya 464-8601

5Rutherford Appleton Laboratory, Chilton, Didcot,Oxfords hire OX110QX, UK

6Department of Physics,Universityof Lethbridge, 4401 Univ ersity Drive,Lethbridge, AlbertaT1J 1B1, Canada

7Astrophysics Group, Department of Physics, The OpenUniver sity, MiltonKeynes, MK76AA, UK

8Laboratoire d’Astrophysique de Marseille, BP8,Traverse d u Siphon, 13376 Marseille Cedex 12, France

9CEA-Saclay,Service d’Astrophysique, France

10Academia Sinica,Institute of Astronomyand Astrophysics, Taiwan

11Department of Physicsand Astronomy, UCLA,Los Angeles, CA, 90095-1547 USA

12Department of Physics& Astronomy, FPRD,Seoul National Uni versity, Shillim-Dong,Kwanak-Gu, Seoul 151-742, Korea

13Spitzer Science Center,California Institute ofTechnolog y, Pasadena, CA91125

14Department of Astronomical Science,The Graduate Universi tyfor Advanced Studies

15Physics Section,Facultyof Humanities and SocialSciences , Iwate University, Morioka, 020-8550

16TOMER&D Inc. Kawasaki, Kanagawa 2130012, Japan

17Asahikawa National College of Technology, 2-1-6 2-joShunk ohdai, Asahikawa-shi, Hokkaido 071-8142

Received September 15, 2009; accepted December 16, 2009

ABSTRACT

Aims.Dust-obscured star-formation becomes much more important with increasing intensity, and increasing redshift. We aim to

reveal cosmic star-formationhistoryobscured bydust usin g deep infraredobservation withthe AKARI.

Methods. We construct restframe 8 µm, 12µm, and total infrared (TIR) luminosity functions (LFs) at 0.15< z <2.2using 4128

infraredsources intheAKARINEP-Deepﬁeld.Acontinuous ﬁl tercoverage inthemid-IRwavelength(2.4,3.2,4.1,7,9,11 , 15,18,

and 24µm) by the AKARI satellite allows us to estimate restframe 8 µm and 12 µm luminosities without using a large extrapolation

based ona SEDﬁt,which was the largestuncertainty inprevio us work.

Results. Wehavefoundthatall8 µm(0.38< z <2.2),12µm(0.15< z <1.16),andTIRLFs( 0.2< z <1.6),showacontinuous

andstrongevolutiontowardhigher redshift.Intermsofcos micinfraredluminositydensity( ΩIR),whichwasobtainedbyintegrating

analytic ﬁts to the LFs,we found a good agreement withprevio us work at z <1.2. We found the ΩIRevolves as ∝(1+z)4.4±1.0.

Whenweseparatecontributionsto ΩIRbyLIRGsandULIRGs,wefoundmoreIRluminoussourcesareinc reasinglymoreimportant