VLBI Observations of HI in Compact Symmetric Objects: the case of B
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1 VLBI Observations of HI in Compact Symmetric Objects: the case of B Esteban D. Araya NRAO Jansky Fellow University of New Mexico Ylva Pihlstrӧm (UNM, NRAO) Greg Taylor (UNM, NRAO) Cristina Rodriguez (UNM) Steven Tremblay (UNM) Rene Vermeulen (ASTRON) NRAO Postdoctoral Symposium, April, 2009
2 20 pc B , VLBA, 15GHz, Taylor et al. (1996)
3 Compact Symmetric Objects (CSOs) - Compact (< 1kpc) radio emission - S-shape morphology - Radio lobes at both sides of a central engine - Radio bright (L5GHz > 5 x 1025 W Hz-1) - GigaHertz Peak Spectrum (GPS) - Elliptical galaxies (but also quasars and spiral galaxies!) - Non-variable, low polarization - No superluminal motions; dynamically young, (<105 yr) Wilkinson et al. (1994) Readhead et al. (1996) Taylor et al. (1996) Augusto et al. (2006)
4 Compact Symmetric Objects (CSOs) - Compact (< 1kpc) radio emission - S-shape morphology - Radio lobes at both sides of a central engine - Radio bright (L5GHz > 5 x 1025 W Hz-1) - GigaHertz Peak Spectrum (GPS) - Elliptical galaxies (but also quasars and spiral galaxies!) - Non-variable, low polarization - No superluminal motions; dynamically young, (<105 yr) Wilkinson et al. (1994) Readhead et al. (1996) Taylor et al. (1996) Augusto et al. (2006)
5 Compact Symmetric Objects (CSOs) - Compact (< 1kpc) radio emission - S-shape morphology - Radio lobes at both sides of a central engine - Radio bright (L5GHz > 5 x 1025 W Hz-1) - GigaHertz Peak Spectrum (GPS) - Elliptical galaxies (but also quasars and spiral galaxies!) - Non-variable, low polarization - No superluminal motions; dynamically young, (<105 yr) - High detection rate of HI absorption (~50%) Wilkinson et al. (1994) Readhead et al. (1996) Taylor et al. (1996) Augusto et al. (2006)
6 Compact Symmetric Objects (CSOs) - Compact (< 1kpc) radio emission VLBI HI Observations: - S-shape morphology - Radio lobes at both sides of a central engine - Radio bright (L5GHz > 5 x 1025 W Hz-1) - GigaHertz Peak Spectrum (GPS) B C C PKS Elliptical galaxies (but also quasars and spiral galaxies!) - Non-variable, low polarization - No superluminal motions; dynamically young, (<105 yr) - High detection rate of HI absorption (~50%) Wilkinson et al. (1994) Readhead et al. (1996) Taylor et al. (1996) Augusto et al. (2006)
7 VLBI HI Observations of CSOs: B , 4C 31.04, 4C 37.11, PKS Arecibo, Mirabel (1990) VLBA, 5GHz, Iν = 20.6 mjy/b, Θsyn = 2 mas, rms = 0.2 mjy/b Giovannini et al. (2001)
8 VLBI HI Observations of CSOs: B , 4C 31.04, 4C 37.11, PKS Arecibo, Mirabel (1990) Conway (1999) VLBA, 5GHz, Iν = 20.6 mjy/b, Θsyn = 2 mas, rms = 0.2 mjy/b Giovannini et al. (2001)
9 B
10 B : Radio Continuum Wilkinson et al. (1994) 18cm, global VLBI SED Peak: ~ 1 GHz Modest Variability < 20% L5GHz ~ 1026 h-2 W Hz-1 Dynamic age ~ 1000 yr Taylor et al. (2000), VLBA
11 B : Other wavelengths Elliptical Galaxy z = σ = 201 ± 17 km/s Mv = mv = 20.1 No IRAS detection (at the Arp220 luminosity limit) X-Ray detection: 0.66 ± 0.27 x 1022 cm-2 absorption column density NED, Palomar, 6450A Readhead et al. (1996) Snellen et al. (2003) Vink et al. (2006)
12 B : Prior HI Observations Vermeulen et al. (2003) WSRT
13 B : Observations + VLBA WSRT - 2 days, ~17 h on source - νsky = MHz - BW = 8 MHz, 1024 channels Dual polarization Final spectral resolution = 15.6 khz (4.1 km/s) Flux density calibration: 2.55 Jy at 1.14 GHz assumed.
14 B : Results Narrow Line: FWHM = 13 ± 2 km/s, NH = 7.3 ± 1.0 x 1021 cm-2 Broad Line: FWHM = 85 ± 4 km/s, NH = 5.2 ± 0.2 x 1022 cm-2
15 B : Continuum Emission toward the HI Absorption
16 B : Continuum Emission toward the HI Absorption (Taylor et al. 1996)
17 B : Radio Continuum toward the HI Absorption (Taylor et al. 1996)
18 B : Nature of the HI Absorption (Taylor et al. 1996)
19 B : Nature of the HI Absorption (Taylor et al. 1996)
20 B : Possible Velocity Gradient
21 B : Possible Velocity Gradient
22 B : Possible Velocity Gradient
23 B : Disk/Torus Interpretation
24 B : Disk/Torus Interpretation Physically Reasonable: MBH ~ 108 M
25 B : Disk/Torus Interpretation Physically Reasonable: MBH ~ 108 M
26 B : Disk/Torus Interpretation Physically Reasonable: MBH ~ 108 M - HI Distribution
27 B : Disk/Torus Interpretation Physically Reasonable: MBH ~ 108 M - HI Distribution - VLBA vs WSTR flux density
28 WSRT Vermeulen et al. (2003) VLBA
29 B : Disk/Torus Interpretation Physically Reasonable: MBH ~ 108 M - HI Distribution - VLBA vs WSTR flux density
30 B results versus other VLBI HI studies CSO
31 B results versus other VLBI HI studies CSO NonCSO
32 B results versus other VLBI HI studies CSO NonCSO
33 Implications for the Study of the MBH - σ* Relation MBH from VLBA HI Observations: ~108 M....
34 Implications for the Study of the MBH - σ* Relation MBH from VLBA HI Observations: ~108 M.... MBH from MBH - σ* Relation: 1.2 x 108 M
35 Summary 1. Compact Symmetric Objects may be the precursors of bright radio galaxies.?
36 Summary 1. Compact Symmetric Objects may be the precursors of bright radio galaxies. 2. Broad HI absorption in B is likely associated with a disk/torus.
37 Summary 1. Compact Symmetric Objects may be the precursors of bright radio galaxies. 2. Broad HI absorption in B is likely associated with a disk/torus. 3. Five CSOs have been imaged in HI at high angular resolution. Conway (1999) B C C PKS B
38 Summary 1. Compact Symmetric Objects may be the precursors of bright radio galaxies. 2. Broad HI absorption in B is likely associated with a disk/torus. 3. Five CSOs have been imaged in HI at high angular resolution. 4. VLBI observations of CSOs may become a powerful tool to investigate the MBH σ* relation. MBH σ*
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