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Radio Selected Damped Lyman Systems. Jeremy Darling (CASA, University of Colorado). Outline: 1. Damped Lya Systems 2. Motivation 3. Intervening Absorption 4. Intrinsic Absorption [5. H 2 CO Absorption] 6. Summary. Damped Lyman Systems. By definition, - PowerPoint PPT Presentation
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Outline: 1. Damped Lya Systems 2. Motivation 3. Intervening Absorption 4. Intrinsic Absorption
[5. H2CO Absorption] 6. Summary
Jeremy Darling (CASA, University of Colorado)
Radio Selected Damped Lyman Systems
Damped Lyman Damped Lyman Systems Systems
By definition,
For the 21 cm HI line,
In practice, we’ll refer to DLAs as any sufficient column, regardless of host or setting.
NHI ≥ 2 1020 cm-2
NHI = 1.8 1018 cm-2 (Tspin / ) d
DLAs: DLAs: Motivation for 21 cm SearchesMotivation for 21 cm Searches
Optical spectroscopic selection: Requires background UV source Redshift into atmospheric window (z > 1.65) Pencil beam (single los, single cloud)
DLA studies: Damped/saturated line (very important for EOR studies!) Optical identification of DLAs
Molecular absorption: Extremely rare Requires dust Fundamental physics Gastrophysics
DLAs: DLAs: Motivation for 21 cm SearchesMotivation for 21 cm Searches
Optical spectroscopic selection: Requires background UV source Redshift into atmospheric window (z > 1.65) Pencil beam (single los, single cloud)
DLA studies: Damped/saturated line (very important for EOR studies!) Optical identification of DLAs
Molecular absorption: Extremely rare Requires dust Fundamental physics Gastrophysics
HI 21 cm: Dust! Any z Multiple los, clouds (+ Einstein rings!)
21 cm HI: = 0.01-0.10 (cf Radio Probes of Reionization, 2007)
Optically faint QSOs
All molecular absorbers show HI 21 cm absorption
Molecular Absorbers: Molecular Absorbers: The Usual Suspects The Usual Suspects
Molecular Absorbers: Four known at z > 0.2
(OH only excluded) Large searches have produced no new objects Molecular Absorption Requires fortuitous alignment Requires flat or inverted continuum Detectability is independent of redshift
Gastrophysics Provides only means to detect unexceptional ISM at z > 0
Precision Measurements Can measure fundamental constants at high redshift
Molecular Absorption Systems at z > 0.2 Molecular Absorption Systems at z > 0.2
• PKS 1413+135 z = 0.2467 AGN in spiral
• B3 1504+377 z = 0.6734 AGN in spiral
• B 0218+357 z = 0.6847 Lens (Einstein ring)
• PKS 1830-211 z = 0.8858 Lens (Einstein ring)
Wiklind & Combes
1998
Wiklind & Combes
1996
Wiklind & Combes
1995
Wiklind & Combes
1997
Kanekar et al 2003
Kanekar et al 2003
Darling (in prep)
Darling (in prep)
Darling (in prep)
Darling (2004)
Conjugate OH lines
No “main” lines
Molecular Absorption Systems at z > 0.2 Molecular Absorption Systems at z > 0.2
• PKS 1413+135 z = 0.2467 AGN in spiral
• B3 1504+377 z = 0.6734 AGN in spiral
• B 0218+357 z = 0.6847 Lens (Einstein ring)
• PKS 1830-211 z = 0.8858 Lens (Einstein ring)
Wiklind & Combes
1998
Wiklind & Combes
1996
Wiklind & Combes
1995
Wiklind & Combes
1997
Kanekar et al 2003
Kanekar et al 2003
Darling (in prep)
Darling (in prep)
Darling (in prep)
Darling (2004)
Conjugate OH lines
No “main” lines
PKS 1413+135: PKS 1413+135: OH and HI AbsorptionOH and HI Absorption
OH satellite lines:1612, 1720 MHz(see also Kanekar et al. 2004)
Systematic offset from HI
Is the offset physical?
How to assess offsets?
13 km s-1
PKS 1413+135: PKS 1413+135: OH, HI & COOH, HI & CO
HI, CO redshifts exceptionally well measured (< 10-6); systematics dominate (Carilli et al. 1998)
OH: Systematic offset from HI, CO
OH-only measure consistent with zero
Δν/HI: systematics can account for all Δα/αo
(1×10-5 ~ 10 km s-1)
HI: Darling 2004OH: Darling 2004CO: Wiklind & Combes 1997
PKS 1413+135: PKS 1413+135: OH, HI & COOH, HI & CO
HI, CO redshifts exceptionally well measured (< 10-6); systematics dominate
OH: Systematic offset from HI, CO
OH-only measure consistent with zero
Δν/HI: systematics can account for all Δα/αo
Intervening 21 cm Absorption:Intervening 21 cm Absorption:A “blind” survey at Green BankA “blind” survey at Green Bank
Goals: Conduct a DLA search analogous to optical surveys (large ∆z). Minimize DLA selection biases (z, dust).
Requires: Large instantaneous z coverage Good velocity resolution (∆v < 10 km s-1) Sensitivity to all DLAs in short integrations
Bonus: Simultaneous search for OH lines Two Surveys: 1. 100 continuum sources (S > 0.8 Jy) in 0.6 < z < 1.1 (Darling & Giovanelli)
2. 182 flat-spectrum sources from z = 0 to z = zsys (Bolatto & Darling)
Feed Resonance
Green Bank Blind HI Survey:Observe 200 MHz at 800 MHz with 6 kHz (~2 km s-1) resolution
λ /Δλ = 132,000
BW/λ = 0.25
Radio Freq Interference (RFI) is problematic andreduces z coverage
RFI
z = 1.1z = 1.1ttll = 8.1 Gyr = 8.1 Gyr
ttUU = 5.6 Gyr = 5.6 Gyr
z = 0.63z = 0.63ttll = 5.9 Gyr = 5.9 Gyr
ttUU = 7.8 Gyr = 7.8 Gyr2.2 Gyr, 1.2 Gpc
Chengalur, deBruyn, & Narasimha 1999
Patnaik et al. 1994
Nair et al. 1993
FWHM = 57 km s-1
τc = 0.22
NHI = 24.3 x 1018 (Ts/f) cm-2
Pure radio HI absorption detection!
Proof-of-concept for blind searches.
• Molecules?• Lens?
Green Bank Blind HI Survey
PKS 1830-211
Chengalur, deBruyn, & Narasimha 1999
Patnaik et al. 1994
Nair et al. 1993
FWHM = 57 km s-1
τc = 0.22
NHI = 24.3 x 1018 (Ts/f) cm-2
PKS 1830-211
Pure radio HI absorption detection!
Proof-of-concept for blind searches.
• Molecules?• Lens?
Green Bank Blind HI Survey
BIMA (Bolatto)
Intervening 21 cm Absorption:Intervening 21 cm Absorption:A “blind” survey at Green BankA “blind” survey at Green Bank
Goals: Conduct a DLA search analogous to optical surveys (large ∆z). Minimize DLA selection biases (z, dust).
Requires: Large instantaneous z coverage Good velocity resolution (∆v < 10 km s-1) Sensitivity to all DLAs in short integrations
Proof of Concept: Detection of 2351+456 at z = 0.78 (no a priori knowledge of this DLA)
Recovery of known absorbers Expectations: ∆z ~ 150 (including RFI losses)
Estimate of ΩHI (but depends on Tspin)
Intrinsic 21 cm Absorption: Intrinsic 21 cm Absorption: CSOsCSOs
Compact Symmetric Objects: Compact (< 1 kpc) Symmetric (jets) Post-Mergers Inside-out virialization (t ~ 108 yr, Perlman et al 2001) Jet advance shows radio source turn-on Crossing time of nucleus « jet lifetime nucleus at birth of RL AGN
Dust and gas still in cores (yet to be expelled) Peck & Taylor 2002
Intrinsic Absorption: Intrinsic Absorption: Survey ExpectationsSurvey Expectations
DLAs
Observe: 71 sources 0.5 < z < 4 CSOs GPS sources CSS sources Expect: Detect all DLAs in 1-2 hours Bonus: OH lines
Intrinsic AbsorptionIntrinsic AbsorptionExpected HI
Intrinsic AbsorptionIntrinsic AbsorptionExpected HI
Flu
x D
ensi
ty (
Jy)
Barycentric Frequency (MHz)
PKS 0500+019z = 0.58
Previous detection:Carilli et al 1998
Intrinsic Absorption: Intrinsic Absorption: Survey Results Survey Results (so far…)(so far…)
z < 0.7 redetections
Intrinsic Absorption: Intrinsic Absorption: Survey Results Survey Results (so far…)(so far…)
No new detections Previous surveys have 30-50% detection rate atz < 0.7 (Vermeulen et al 2003)
Sub-DLAs detectable
Adequate sensitivity to z ~ 3, including RFI losses
Work continues…
z < 0.7 redetections
HH22CO: CO: The Swiss Army Knife MoleculeThe Swiss Army Knife Molecule
Galactic
Extragalactic
Gastrophysics
Galaxy Evolution
(Cosmology ?)
Darling & Goldsmith (in prep)
NGC 2264
Galactic HGalactic H22CO CO
Dark Clouds: - “Anomalous” H2CO absorption (e.g. Palmer et al.
1969)
- Absorption in multiple cm lines- No radio continuum source!
Darling & Goldsmith (in prep)
Darling & Goldsmith (in prep)
Barnard 227
NGC 2264
HH22CO: CO: The DASARThe DASAR
L ightA mplification byS timulated E mission ofR adiation
Inversion: “Heating” of lines Tx >> Tkin
Pump required: Chemical, collisional, radiative
D arkness*A mplification** byS timulated A bsorption ofR adiation
Townes et al (1953)
Anti-Inversion: “Cooling” of lines Tx < TCMB
Pump required: Collisions with H2
*Not really dark.**Not a true amplification.
Galactic HGalactic H22CO CO
Dark Clouds: - “Anomalous” H2CO absorption (e.g. Palmer et al.
1969)
- Absorption in multiple cm lines- No radio continuum source!
• Can H2CO be observed in other
galaxies?
2. Can “anomalous” H2CO absorption be
observed in galaxy-scale analogs of Dark Clouds?
Darling & Goldsmith (in prep)
Darling & Goldsmith (in prep)
Barnard 227
NGC 2264
Darling & WiklindBiggs et al 2001
Extragalactic HExtragalactic H22CO CO
Maser Emission in (U)LIRGs (OH Megamasers)
Arp 220 III Zw 35
Absorption in starbursts (OH absorbers)
NGC 520NGC 660
Absorption in dense cloudsB0218+357
Ortho-HOrtho-H22CO Toward CO Toward
B0218+357 B0218+357 4.8 GHz (110-111) line detected at Arecibo
• Two gaussian components• app = 0.013 ± 0.003
• ∆v = 12.6 ± 0.6 km s-1
Previous Detections:Previous Detections: 14.5 GHz (211-212) (VLA; Menten & Reid 1996)
150.5 GHz (211-110) (IRAM; Wiklind & Combes)
Wiklind & Combes
Darling & Wiklind
HH22CO Toward B0218+357: Summary CO Toward B0218+357: Summary
Similar to Galactic Dark Clouds (but scaled to CMB at z = 0.67)
• Centimeter lines (4.8, 14.5 GHz) are anti-inverted- T4.8 ~ 2.3 K- T14.5 ~ 3.4 K (TCMB = 4.6 K)
• Millimeter lines (150.5, 140.8 GHz) have Tex ~ TCMB
• N(ortho-H2CO) = 1.5 1013 cm-2 • N(H2) = 1.5 1021-22 cm-2 • n(H2) = 104-5 cm-3
Future Prospects:• Ortho:para at z > 0• Prediction: H2CO can be observed in absorption against CMB in extragalactic ISM
- How does T decrement scale with z? - What is H2CO filling factor?
HH22CO Absorption Against the CMB CO Absorption Against the CMB
HH22CO: CO: The DASARThe DASAR
The CMB is the ultimate illumination source:
• Behind everything• Everywhere• Uniform on arcsec scales
H2CO absorption against the CMB offers an unrivaled probe of dense molecular gas, independent of redshift!
HH22CO Against the CMB: CO Against the CMB: ProspectsProspects
Step 1: Local Calibration• Survey local galaxies, from spirals to ULIRGs• Include sample with CO and HCN measurements• What is the filling factor on kpc scales? • What is the total H2CO mass? M(H2CO) M(dense)
GBT: large survey in 14.5 and 4.8 GHz lines (Darling, Mangum, Menten, & Henkel)
Step 2: Submm Galaxies• How does anti-inversion scale with redshift?• What is dense gas fraction?VLA: deep integrations in 312 - 313 line at z ~ 2.5
(Darling & Baker)
Radio-Selected Damped Lyman Radio-Selected Damped Lyman Systems Systems
New Radio Facilities Allow Optical-Style Surveys• Intervening absorption, independent of dust• Proof of concept detection of DLA• ∆z ~ 150 Intrinsic Absorption • Expect high detection rates• Sensitivie to DLAs to z = 4• OH search for free
Stimulated Absorption by H2CO (DASARs)• Uses CMB as illumination source• Traces gastrophysics in detail • Potentially very large pool of objects to observe (still much foundational/calibration work to be done…)
The End The End
Conjugate OH: Anti-masing Conjugate OH: Anti-masing
Selection rules: ΔF = ± 1,0
Intra-ladder transitions overpopulate F = 2: 1720 emission 1612 absorption
Inter-ladder transitions overpopulate F = 1: 1720 absorption 1612 emission
16121720
Conjugate OH lines:
Conjugate lines in NGC Conjugate lines in NGC 253 253
Frayer, Seaquist & Frail (1998)
Conjugate OH lines show changing structure along line of sight:
1720 emission N(OH)/V < 1015 cm-2 km-1 s N(H2) < 1022 cm-2
1612 emission N(OH)/V > 1015 cm-2 km-1 s N(H2) > 1022 cm-2
Note: Conjugate lines weakly amplify background continuum Detectability follows rules of absorption, not emission
HH22CO Absorption in Dark Clouds CO Absorption in Dark Clouds
“Anomalous absorption” in Galactic dark clouds (Palmer et al 1969)
Tex < TCMB
2 cm lines also observed in absorption against CMB “Anti-inversion” due to collisional pumping (Evans et al 1975)
cm line ratio proxy for n(H2)
2 mm emission observed in Galactic dark clouds (Evans & Kutner 1976)
gastrophysics
HH22CO: The Swiss Army Knife CO: The Swiss Army Knife MoleculeMolecule
Anti-inverted (cm) line ratios yield n(H2), nearly independent of Tkin
Line ratios between species give ortho:para ratio H2CO formation channel (hot/cold; gas/dust)
Line ratios from different Ka
ladders of a given species (ortho/para) yield Tkin
∆J = ±1 line ratios within a Ka ladder yield Trot
Extragalactic HExtragalactic H22CO CO
Maser Emission in (U)LIRGs (OH Megamasers)
Arp 220 III Zw 35
Absorption in starbursts (OH absorbers)
NGC 520NGC 660
Absorption in dense cloudsB0218+357
Darling & Henkel
Baan, Guesten, & Haschick (1986)
Extragalactic HExtragalactic H22CO CO
Maser Emission in (U)LIRGs (OH Megamasers)
Arp 220 III Zw 35
Absorption in starbursts (OH absorbers)
NGC 520NGC 660
Absorption in dense cloudsB0218+357
Filho, Barthel, & Ho (2002)
NGC 660, 8.4 GHz
Darling & Henkel (in prep)
Extragalactic HExtragalactic H22CO CO
Darling & Henkel (in prep)
Maser Emission in (U)LIRGs (OH Megamasers)
Arp 220 III Zw 35
Absorption in starbursts (OH absorbers)
NGC 520NGC 660
Absorption in dense cloudsB0218+357
Filho, Barthel, & Ho (2002)
NGC 660, 8.4 GHz
~350 pc
~375 km/s
Mencl = 1.4109 M
HH22CO: CO: A Planar Asymmetric Top MoleculeA Planar Asymmetric Top Molecule
Wiklind & Combes
HH22CO: CO: Anti-Inversion in Centimeter LinesAnti-Inversion in Centimeter Lines
Allow 4 excitation temps:
1. No physical solution with
Tcm > TCMB
2. No solution with Tmm= Tcm
3. No solution with Tmm= T4.8
4. If T14.5 = T4.8 then all lines
have Tex < TCMB
5. If Tmm ≥ TCMB then
TCMB > T14.5 > T4.8
Chengalur, deBruyn, &Chengalur, deBruyn, & Narasimha 1999Narasimha 1999
Patnaik et al. 1994Patnaik et al. 1994
Nair et al. 1993Nair et al. 1993
PKS 1830-211
Darling (in prep)
Menten et al. 1999300 km/s
Extended Illumination: PKS 1830-211Extended Illumination: PKS 1830-211
PKS 1830-211: - Einstein ring at z = 0.89
- HI and OH absorption
- CO, HCN, HCO+,… absorption
- Moleculear isotope absorption
- H2CO absorption
Scaling Relations Scaling Relations
Detection of cm H2CO Lines vs z Depends on:
• (Anti) Inversion vs z How does Tcm - TCMB scale vs z?
(TCMB = 2.73 (1+z) K)
• Filling factor on kpc scales
• Filling factor vs z
• Angular size vs z
Scaling Relations Scaling Relations
Detection of cm H2CO Lines vs z Depends on:
• (Anti) Inversion vs z How does Tcm - TCMB scale vs z?
Tcm - TCMB (1+z)
• Filling factor on kpc scales
• Filling factor vs z
• Angular size vs z
Scaling Relations Scaling Relations
Detection of cm H2CO Lines vs z Depends on:
• (Anti) Inversion vs z How does Tcm - TCMB scale vs z?
Tcm - TCMB (1+z)
• Filling factor on kpc scales
• Filling factor vs z
• Angular size vs z
Scaling Relations Scaling Relations
Detection of cm H2CO Lines vs z Depends on:
• (Anti) Inversion vs z How does Tcm - TCMB scale vs z?
Tcm - TCMB (1+z)
• Filling factor on kpc scales
• Filling factor vs z
• Angular size vs z - CMB power in small beams
Rayleigh-Jeans Law
CMB power scales as beam
arcmin:arcsec 3600:1
~100 mJy ~30 µJy
HH22CO Against the CMB: CO Against the CMB: ProspectsProspects
The Future:
- Molecule of choice for studies of star formation, molecular gas from present day to arbitrary redshift
EVLAALMAHigh Sensitivity Array
Ortho:Para H2CO gives astrochemistry channel(dust vs gas, hot vs cold)
H2CO mm + cm lines yield gastrophysicsTkin n(H2) Tx TCMB
No redshift limit to detection (in fact, angular size grows at high z)
HH22CO as z-Machine CO as z-Machine
If H2CO can be observed against the CMB, • Anti-inversion obviates need for chance alignments• Unique probe of gastrophysics of dense molecular ISM
Much foundational work yet to be done… Scaling relations Filling factor on kpc scales Total H2CO mass in galaxies: M(H2CO) M(dense)
Regardless, H2CO should be observable with ALMA:• Absorption and emission• Similar abundance, line luminosity to HCN (~10%)• Ortho:para H2CO at z > 0• Line Tex floor set by CMB, scales with z
Pathologies as Probes Pathologies as Probes
Masers provide exceptional Tb • Precision positions (H2O in NGC 4258)• Probes of intervening gas (scintillation)• Signposts at cosmological distances Tunneling • NH3 is a maser and molecular ISM thermometer
Conjugate Lines• Local H2 density indicator• Probe of fundamental physical constants
Stimulated Absorption (DASARs)• Uses CMB as illumination source• Traces gastrophysics in detail • Potentially very large pool of objects to observe (still much foundational/calibration work to be done…)