paola%andreani,edwin%retana1montenegro, zhi1yu%zhang ... · gravitational lenses paola%andreani...

Paola Andreani, Edwin Retana-‐Montenegro,Zhi-‐Yu Zhang, Padelis Papadopoulos, Chentao Yang, Simona Vegetti

Paola AndreaniAPEX Band5, ESO, Feb 1-‐3

Gravitational Lenses

Paola Andreani

HATLAS SDP FIELD

Negrello et al., 2007, 2010

Gravitational Lenses

Paola Andreani

HATLAS SDP FIELD

Canalog+, 2015

Keck K-‐band

Ma+,2015Keck K-‐band + IRAC

A zoomed view on G12v2.43

Paola Andreani

11h35m20s24s28s32s

RA (J2000)

4800000

4700000

4600000

4500000

�1�4400000

Dec

(J20

00)

APEX Band5, ESO, Feb 1-‐3

Paola AndreaniAPEX Band5, ESO, Feb 1-‐311h45m40s46m00s20s40s47m00s20s

RA (J2000)

2400000

1800000

1200000

�0�0600000

+0�0000000

Dec

(J20

00)

Zooming into G12v2.30

H2O1mm

13h29m30s30m00s30s31m00s

RA (J2000)

+24�4800000

5400000

+25�0000000

0600000

1200000

Dec

(J20

00)

Zooming into NBv1.78


H2O1mm

APEX Band5, ESO, Feb 1-‐3 Paola Andreani

• 3P fine structure [CI] lines • @ 492.2 and 809.3 GHz • nc ~ 500 and 103 cm-‐3

• Optical thin

• well mixed with all the CO-‐rich H2 à a good H2 bulk mass tracer (Papadopoulos et al. 2004)

• positive K correction at high z's over the low-‐J CO lines • Trace the CO invisible H2 gas where Cosmic Rays from SN destroy CO and leave behind C (Bisbas et al. 2015) • less affected by the CMB effect


• 3P fine structure [CI] lines • @ 492.2 and 809.3 GHz • nc ~ 500 and 103 cm-‐3

• Optical thin

• well mixed with all the CO-‐rich H2 à a good H2 bulk mass tracer (Papadopoulos et al. 2004)

• positive K correction at high z's over the low-‐J CO lines • Trace the CO invisible H2 gas where Cosmic Rays from SN destroy CO and leave behind C (Bisbas et al. 2015) • less affected by the CMB effect


Zhang et al., 2016

• ISM energy supply : few CO lines (high-‐J CO lines as CO 7-‐6, and low-‐J ones like CO 1-‐0, 2-‐1)• Comparison CO J=7-‐6 luminosity vs CO 1=1-‐0 or vs CI(1-‐0) CI(2-‐1)• insights on whether FUV-‐photons from SF regions power the molecular gas• whether other, more powerful and global heating mechanisms of H2 are needed (Cosmic rays and/or strong turbulence).

• CO(7-‐6)/CI(2-‐1) ratio àMdense,warm(H2)/M_total(H2) tracer• Caveats: CI 2-‐1 (or CI 1-‐0) to be calibrated as H2 global mass tracers



G12v2.30H-ATLAS J114637.9−001132z= 3.2592

NBv1.78H-ATLAS J133008.4+245900z=3.1112

G12v2.43 (H-ATLAS J113526.3−014605Z=3.1276)


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0 5 10 15 20 25 30 35 40 45 50CO76/CO10

Count

G12v2.30

NBv1.78

G12v2.43

Mrk1014IRAS03521IRAS03158Mrk231M82

Mrk273, Arp193, Arp220NGC1266, NGC253, NGC24NGC1614, IRASF01417

IC1623MGC-‐03-‐04ESO244

NGC1068MGC+12IC10, NGC232

NGC828NGC891NGC23

detectionsupper limitsLenses z~3

6.2: MW: Centre

infer the global excitation drivers of the ISM in lenses

Lenses stand in a non-‐FUV territory

CO(7-‐6)CO(1-‐0)

Paola AndreaniAPEX Band5, ESO, Feb 1-‐3Data from Kamenetzky et al., 2014; Israel et al. 2015

SDP.9

SMGs

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0 1 2 3 4 5 6 7 8 9 10 11 12CO76/CI21

Count

G12v2.30

G12v2.43

MCG+12

M82, Mrk231, Mrk273, Arp220NGC253, IRASF01417, NGC0958NGC1614, NGC1614

NGC1377, UGC02608, UGC03094UGC02238, NGC891, NGC8773C84, ESO353, ESO420, NGC1961NGC1068, NGC1482, NGC1052

NGC1222, MCG-‐02, IC10, Mrk1014UGC01845, Arp193, NGC23, I-‐Zw-‐1NGC232, NGC4051, NGC0695, NGC1572

Cen ANGC1097NGC205

detectionsupper limitslenses z~3

M 17

NBv1.78

CO(7-‐6)CI(2-‐1)

Paola AndreaniAPEX Band5, ESO, Feb 1-‐30.9: MW: Centre


Atomic C column density

CO column density

Constant flux ratio CO(7-‐6)/CI(2-‐1)

Tk = 25 Klog(nc) = 4.5 cm-3

Israel+, 2015

[CI] emission arises from a dense and warm gas,~10-‐20% of the C in gas phase

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-6.5 -6.0 -5.5 -5.0 -4.5 -4.0 -3.5 -3.0 -2.5LCO76/LFIR

Count

G12v2.43

G12v2.30NBv1.78

L CO(7-‐6) (L ⦿) / L (FIR) (L ⦿)

NGC1097

NGC891Cen A

UGC02238UGC02608UGC030094

NGC1222NGC1377

Arp220NGC1056NGC23

NGC1266

M82NGC4051Mrk231Mrk2733C84NGC253NGC232IRAS03158NGC1068

NGC1572Arp193ESO353

LCO(7-‐6)L(FIR)



Rosenberg et al., 2015

A single component theoretical PDR modelcannot match these flat SLED shapes

Additional heating mechanism necessaryto explain the observed molecular emission


Rosenberg et al., 2015

A single component theoretical PDR modelcannot match these flat SLED shapes

Additional heating mechanism necessaryto explain the observed molecular emission

Oteo et al., 2017

• 3 lensed z~3 galaxies observed and detected with APEX/SEPIA 5• CO(7-‐6) has been detected in all 3 objects• CI[2-‐1] in 2 out of 3

• The analysis of the ratios CO(7-‐6)/CI[2-‐1], CO(7-‐6)/CO(1-‐0) and CO(7-‐6)/L(FIR) shows:• These 3 objects locate far away from FUV dominated excitation and other excitation mechanism need to be acting.

• Differential lensing magnification needs to be investigated if the distribution of the warm and cold dust is different

• Consequences• If strong turbulence and/or high CR energy densities responsible for the large amounts of very warm and dense gas initial conditions of SF may change.

• the wide range of average ISM conditions will strongly impact the so-‐called Xcofactor and the determination of the amount of molecular gas


paola%andreani,edwin%retana1montenegro, zhi1yu%zhang ... · gravitational lenses paola%andreani...

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