june 4, 2015dusty2004 spitzer space telescopecen a elliptical and (other) early-type galaxies t....
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![Page 1: June 4, 2015Dusty2004 Spitzer Space TelescopeCen A Elliptical and (other) early-type galaxies T. Wiklind ESA/STScI](https://reader035.vdocuments.mx/reader035/viewer/2022062714/56649d2c5503460f94a01827/html5/thumbnails/1.jpg)
April 18, 2023 Dusty2004Spitzer Space TelescopeCen A
Elliptical and (other) early-type galaxies
T. WiklindESA/STScI
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April 18, 2023 Dusty2004Spitzer Space TelescopeCen A
1. Cold gas in elliptical/S0 galaxies• What we know today
2. What are the issues?• Origin of early-type galaxies?• Relation between AGN and dense gas?• Connection with cooling flows• Cold dust
3. Observations needed for progress• Herschel• ALMA
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April 18, 2023 Dusty2004
The gas content of elliptical galaxies
Elliptical galaxies are gas-rich objects
Type of gas
Temp
K
Density
cm-3
Mass
Mo
Fraction
Hot 107 0.1 1010 >0.8
Warm 104 102 104 - 105 >0.5
Cool 102 102 - 103 107 - 1010 0.1 - 0.2
Dust <102 >103 105 - 107 ~0.8
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April 18, 2023 Dusty2004
Cold ISM in lenticular galaxies:
Atomic hydrogen:
Molecular hydrogen:
Dust emission:
30-40% of far-infrared selected S0’s
25% of far-infrared selected S0’s
40-60% at 100m (IRAS)Optical features (?)
Main problem: no unbiased (or with biased controlled) survey hasbeen done to date.
Needed: survey with well-defined mass limitpreferably without far-infrared bias
One study has been done with a volume limited sample: S0, <20 Mpc, non-peculiar,non-Virgo Detection rate ~80% for CO emission (Welch & Sage 2003).No correlation between molecular mass and blue luminosity.
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April 18, 2023 Dusty2004
Oosterloo et al. 2002
HI in dust-lane ellipticals:
Regular HI disks, extended well outside the optical boundary.Well-behaved kinematics.Long-lived features.
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April 18, 2023 Dusty2004
NGC759 CO(1-0)observed with PdB(Wiklind et al. 1997)
Unresolved CO emission, implying > 109 Mo
of molecular gas gas ring with r~3” inferredand confirmed optically (B-I image)(Vlasyuk & Sil’chenko 2000)
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April 18, 2023 Dusty2004
NGC759 observed with Plateau de Bure(Wiklind et al. 1997)
Unresolved CO emission, implying > 109 Mo
of molecular gas gas ring with r~3” inferredand confirmed optically (B-I image)(Vlasyuk & Sil’chenko 2000)
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April 18, 2023 Dusty2004
Gas in lenticulars(Pogge & Eskridge 1998)
Molecular gas has the samedistribution as the ionized gaswhile HI can be extended.
Some lenticulars with atomicgas show no evidence of starformation (Pogge & Eskridge 1998)
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April 18, 2023 Dusty2004Blue cores in early-types(de Mello et al. 2004)
GOODS/ACS I
zphot ~ 0.6
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April 18, 2023 Dusty2004
GOODS/ACS I + B + WFPC2 U
Blue cores in early-types(de Mello et al. 2004)
zphot ~ 0.6
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April 18, 2023 Dusty2004
The origin of elliptical galaxies
• Elliptical galaxies contain an old stellar population, necessarilyformed at high z
• Two formation scenarios:(1) monolithic collapse at early times, followed by passive evolution(2) hierarchical merging, with rather late formation epoch
• Very luminous galaxies with extreme star formation rates arefound in submm surveys at redshifts 2-3
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April 18, 2023 Dusty2004
Cimatti et al. 2004
Four elliptical galaxies at z = 1.6 - 1.9Spectroscopically confirmedAges ~1-1.7 Gyr (zf ~ 3)M* ~ 1-3 1011 Mo
Too few such systems arepredicted in hierarchical models
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April 18, 2023 Dusty2004
Chandra Deep Field Southincluding parts of GOODS-Sand UDF
SIMBA observation =1200mrms ~0.5 mJy/beam
Bergström et al. 2004
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April 18, 2023 Dusty2004
Excellent fit:Starburst galaxy at z>7, SFR ~ 500 Mo/yr; M* ~ 1012 Mo
Age ~ 0.5 Gyr
Not so good fit:Evolved elliptical at z~3Passive evolution, no star formationAge ~ 1-2 Gyr (zf ~ 5-7)
A proto-elliptical at z>7?
Submm galaxies at high redshift :
• High star formation rates ~103 Mo/yr (or more)• Massive systems with gas masses ~1010-1011 Mo (CO observations)• If SFR sustained ~108 yrs they will form ~1011 Mo in stars
For more info:Mobasher et al. 2004
Submm galaxies could be proto-ellipticals forming througheither monolithic collapse or major merger events
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April 18, 2023 Dusty2004
Images from John Hibbard’sweb pagehttp://www.cv.nrao.edu/~jhibbard/
Central 7” of NGC 7252 with HST/WFPC2Whitmore et al. 1992
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April 18, 2023 Dusty2004
• About 15% of radio galaxies contain a coldISM (molecular gas+dust). Same as FIRselected E (Lima et al 2000; Leon et al. 2002)
• Both centrally concentrated and extended gasdistributions with masses from ~108 - 1010 Mo
• Despite large gas masses RG fall on theFundamental Plane
• No clear correlation with LB.
• Correlation with AGN activity? Most RG’sdo not have significant amounts of cold gas…
• Six high redshift radio galaxies have beenfound to contain molecular gas (z=0.2 - 3.8)(Papadopoulos et al. 2000; de Breuck et al 2003; Greve et al. 2004).
• HzRG may be starburst galaxies: largemolecular gas mass (1011 Mo) and highLFIR (>1012 Lo)
Radio galaxies
Low redshift High redshift
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April 18, 2023 Dusty2004
• NGC1275 (Per A) contains >109 Mo of molecular gas, but unknownif connected to cooling flow or on-going merger (Lazareff et al. 1989)
• Molecular gas has recently been detected in 16+ cooling flow galaxies(Edge et al. 2001; Salome & Combes 2003, 2004)
• Molecular gas masses are 108 - 1010 Mo, too small to account for totalcooling flow deposition
• Strong correlation between moleculargas and H emission (Salome &Combes 2003)
• Less strong correlation betweenmolecular gas mass and massdeposition rates (but only thecentral part observed)
Molecular gas in cooling flow galaxies
Salome & Combes 2003
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April 18, 2023 Dusty2004
• Dust emission is detected in many cooling flow (e.g. Edge et al. 1999)
• Heating by AGN or star formation?
• IRAM PdB images show extended CO(1-0) and CO(2-1) emissionin A1795. Apparently along the radio jet (Salome & Combes 2004).
Molecular gas in cooling flow galaxies contd.
Salome & Combes 2004
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April 18, 2023 Dusty2004
• IRAS detected emission in ~40% of elliptical galaxies (Knapp et al. 1986)Md ~ 105 - 107 Mo, Td ~ 30K
• ISO sample of 54 early-type galaxies (39 E’s) with detection rate ~50%(Temi et al. 2004). ISO + SCUBA gives similar result (Leeuw et al. 2004)
• FIR luminosity not well correlated with optical luminosities (same as IRAS results)
• Two dust components:(1) A warm component with Td ~ 40 K(2) A cool component with Td ~ 17-20 K
• Total dust mass 10x larger than inferred from IRAS data
• With ~constant gas-to-dust mass ratio, more cold molecular gas is implied
Dust in elliptical galaxies
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April 18, 2023 Dusty2004
Leeuw et al. 2002
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April 18, 2023 Dusty2004
What can Herschel and ALMA do?
ALMA
Distribution and kinematics of molecular gas in ellipticals(study the structure of E potential)
- Radio galaxies: is the molecular gas Necessary for activity?
- Cooling flows: How is the gas related to the hot gas? Is it forming stars? Where does it form?
Molecular gas in ellipticals as a functionof redshift. Merger rate?(need HST/JWST for morphology)
Herschel
Complete and unbiased surveys of coldISM in ellipticals / radio galaxies
Detailed SEDs (+ long bolometers) toderive dust components/mass
Fine-structure lines to study the physicsof the cool ISM/star formation (Malhotraet al. 2000)
Occurance of hot/cold dust in cooling flowsdistribution / heating agent