Imaging nearby AGN at ultra high resolution with RadioAstron Tuomas Savolainen Aalto University Metsähovi Radio Observatory Max-Planck-Institut für Radioastronomie.

Slides:



Advertisements
Similar presentations
AGN9, Ferrara Maggio 2010 Gabriele Bruni – IRA INAF, Univ. Bologna A RADIO APPROACH TO BROAD ABSORPTION LINE QUASARS Gabriele Bruni (IRA-INAF, Univ.
Advertisements

1 RA III - Regional Training Seminar on CLIMAT&CLIMAT TEMP Reporting Buenos Aires, Argentina, 25 – 27 October 2006 Status of observing programmes in RA.
Wide Field VLBI Imaging I (Background) Indra Bains.
HI absorption around the nucleus of an active galaxy NGC1052 Yun-da Li Supervisor : Sawada-Satoh, Satoko Shen, Zhiqiang August 28, 2003 ASIAA summer student.
Probing the Radio Counterpart of Gamma-ray Flaring Region in 3C 84 Hiroshi Nagai (National Astronomical Observatory of Japan) In collaboration with Monica.
Kinematic Studies of the IDV Quasar S. Bernhart T. P. Krichbaum L. Fuhrmann Max-Planck-Institut fϋr Radioastronomie, Bonn.
Gabriele Giovannini Dipartimento di Astronomia, Bologna University Istituto di Radioastronomia - INAF EVN observations of M87 as follow-up on a recent.
Gabriele Giovannini Dipartimento di Astronomia, Bologna University Istituto di Radioastronomia - INAF The jet and core in M 87 In collaboration with :
Mapping HI absorption at z=0.026 against a resolved background CSO Andy Biggs, Martin Zwaan, Jochen Liske European Southern Observatory Frank Briggs Australian.
M87 - WalkerVSOP-2 Symposium, Sagamihara, Japan Dec IMAGING A JET BASE - PROSPECTS WITH M87 R. Craig Walker NRAO Collaborators: Chun Ly (UCLA - was.
A Polarization Study of the University of Michigan BL Lac Object Sample Askea O'Dowd 1, Denise Gabuzda 1, Margo Aller University College Cork 2 -
VLBA polarimetry of the Fermi-detected quasar B : a rare “spine and sheath” polarisation structure Jun Yang (JIVE, Netherlands) Alaxander B. Pushkarev.
Very Long Baseline Interferometry (VLBI) – Techniques and Applications Steven Tingay ATNF Astronomical Synthesis Imaging Workshop Narrabri, 24 – 28 September,
THE SEARCH OF GIANT RADIO GALAXIES AT DECLINATIONS FROM 3 TO 12 DEGREES Pushchino Radio Astronomy Observatory of Astro Space Center Tyul’bashev S.A., Gliantsev.
4/19/2017 7:18 PM Linear and circular radio and optical polarization studies as a probe of AGN physics I. Myserlis E. Angelakis (PhD advisor), L. Fuhrmann,
Super-resolution imaging with Sparse Modeling Mareki Honma (NAOJ) Kazu Akiyama(U. Tokyo) Makoto Uemura (Hiroshima U.) Shiro Ikeda (Institute of Statistical.
Sub-mm VLBI for resolving super-massive black hole Mareki Honma VERA / Mizusawa VLBI observatory, NAOJ.
An idea of Space mm/sub- mm VLBI Array Xiao-Yu Hong ( 洪晓瑜 ) Jun-Hui Zhao ( 赵军辉 ) Zhi-qiang Shen ( 沈志强 ) Shanghai Astronomical Observatory ( 中国科学院上海天文台.
Deep, wide-field global VLBI observations of HDF-N Deep, wide-field global VLBI observations of HDF-N Seungyoup Chi Kapteyn Institute (RuG) / JIVE Collaborators.
Direct imaging of AGN jets and black hole vicinity Tiziana Venturi Active Galactic Nuclei 9 Ferrara,
Probing AGN physics with VLBI at Parkes Stas Shabala University of Tasmania.
VSOP-2 Detection of Faraday screen? Inoue M., Asada K.*, and Nagai H. National Astronomical Obs. of Japan * Institute of Space and Astronautical Science.
Sándor Frey FÖMI Satellite Geodetic Observatory P.O. Box 546, H-1373 Budapest, Hungary Space VLBI.
Imaging Compact Supermassive Binary Black Holes with VLBI G. B. Taylor (UNM), C. Rodriguez (UNM), R. T. Zavala (USNO) A. B. Peck (CfA), L. K. Pollack (UCSC),
Which dipoles to use to optimize survey speed? –What tapering? –Trade-off between sensitivity, FOV and low side-lobe levels –Station beam stability, pointing.
(Spectral Line) VLBI Chris Phillips CSIRO ATNF Chris Phillips CSIRO ATNF.
The jet of Mrk 501 from millions of Schwarzschild radii down to a few hundreds Marcello Giroletti INAF Istituto di Radioastronomia and G. Giovannini, G.
VLBI/eVLBI with the 305-m Arecibo Radio Telescope Chris Salter Tapasi Ghosh Emmanuel Momjian Arun Venkataraman Jon Hagen.
Designing Experiments T. Venturi Istituto di Radioastronomia, Bologna, INAF ERIS, Manchester, 9 September 2005.
1 Gbps Disk-Based VLBI Observation for Future East Asia VLBI Observations Kiyoaki Wajima 18 March 2009 동아시아 VLBI 워크샵 Yamaguchi University Introduction.
I.Introduction  Recent evidence from Fermi and the VLBA has revealed a strong connection between ɣ -ray emission in AGNs and their parsec-scale radio.
3C120 R. Craig Walker National Radio Astronomy Observatory Socorro, NM Collaborators: J.M. Benson, S.C. Unwin, M.B. Lystrup, T.R.Hunter, G. Pilbratt, P.E.
Ultra-high Resolution Space-VLBI Imaging of Jets in Nearby AGN Tuomas Savolainen Aalto University Metsähovi Radio Observatory, Finland Max-Planck-Institut.
Four hot DOGs eaten up with the EVN Sándor Frey (FÖMI SGO, Hungary) Zsolt Paragi (JIVE, the Netherlands) Krisztina Gabányi (FÖMI SGO, Hungary) Tao An (SHAO,
Jet dynamics and stability Manel Perucho Universitat de València The innermost regions of relativistic jets and their magnetic fields Granada, June 2013.
Мulti-frequency VLA observations of M87. Observations’ parameters Test VLA observations (configuration D) of M87 (RA=12:28, Dec=12:40) took place on November.
The core shift measurements for two-sided jets affected by Free-Free absorption using VLBA Takafumi Haga (SOKENDAI/ISAS) Collaborators Akihiro Doi, Yasuhiro.
Investigation of different types radio sources by IPS method at 111MHz S.A.Tyul’bashev Pushchino Radio Astronomy Observatory, Astro Space Center of P.N.Lebedev.
The MOJAVE Program: Studying the Relativistic Kinematics of AGN Jets Jansky Postdoctoral Fellow National Radio Astronomy Observatory Matthew Lister.
Young Radio Sources associated with Broad Absorption Line Quasars
RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing,
AGN Science with SKA Motoki Kino (NAOJ) On behalf of SKA-Japan AGN sub-WG Japan-SKA workshop (Nov. 5 th 2010, NAOJ) (C) J. McKean Cygnus A at 240 MHz with.
THE KINEMATICS OF th EVN SYMPOSIUM N.A. Kudryavtseva 1, S. Britzen 1, J. Roland 2, A. Witzel 1, E. Ros 1, A. Zensus 1, A. Eckart 3.
Gabriele Giovannini Marcello Giroletti Gregory B. Taylor Dipartimento di Astronomia, Bologna University Istituto di Radioastronomia, INAF Bologna Dept.
Multi-Frequency Observations of the Gravitational Lens B Anupreeta More Max-Planck-Institut fuer Radioastronomie, Bonn Supervisor : Richard Porcas.
KVN V LBI E xtragalactic Co mpact R adio S ource S urvey Lee, Sang-Sung 2009EastAsiaVLBIWorkshop 2009EastAsiaVLBIWorkshop.
A Global 86 GHz VLBI Survey of Compact Radio Sources Sang-Sung Lee MPIfR In collaboration with A.P. Lobanov, T.P. Krichbaum, A. Witzel, J.A. Zensus (MPIfR,
Marcello Giroletti INAF Istituto di Radioastronomia and
G.Giovannini Department of Physics and Astronomy – Bologna University & IRA/INAF with the collaboration of M. Giroletti, K. Hada and M. Orienti (IRA/INAF)
Quasi-Periodicity in the Parsec-Scale Jet of the Quasar 3C345 - A High Resolution Study using VSOP and VLBA - In collaboration with: J.A. Zensus A. Witzel.
AUSAC March Arecibo Tapasi Ghosh, Chris Salter, Arun Venkataraman Outline: 1. The Present Capability & Operations 2. Post-painting Observations.
E. Momjian, T. Ghosh, C. Salter, & A. Venkataraman (NAIC-Arecibo Observatory) eVLBI with the 305 m Arecibo Radio Telescope ABSTRACT Using the newly acquired.
Dependence of the Integrated Faraday Rotations on Total Flux Density in Radio Sources Chen Y.J, Shen Z.-Q.
VLBI Monitoring of Gamma-Ray Blazar PKS Faith Hungwe (Rhodes/HartRAO) Dr Roopesh Ojha (NASA/GSFC) Prof Roy Booth (HartRAO)
Mapping Magnetic Field Profiles Along AGN Jets Using Multi-Wavelength VLBI Data Mark McCann, Denise Gabuzda Department of Physics, University College Cork,
Next Generation Space VLBI Project: VSOP-2 Inoue, M. 1, Nagai, H. 1, Asada, K. 2, Saito, H. 2, Tsuboi, M. 2, and the Next Generation Space VLBI Working.
How Compact are Blazar Cores – AGN studied with micro- arcsecond/sub-pc scale resolution T.P.Krichbaum with contributions from U. Bach, S. Lee, M. Gurwell.
About JVN about JVN Status Status Results Results Future plans Future plans Japanese VLBI Network (JVN): recent results and future plans for EAVN Kenta.
The Atomic and Molecular Environments of AGN Alison Peck SAO/SMA Project.
EVN 2015 Starburst Galaxies
RadioAstron: deep into AGN jets
L. Kogan (NRAO), S. Likhachev, I. Girin, & V. Ladigin (ASC)
A VLBA MOVIE OF THE JET LAUNCH REGION IN M87
An Arecibo HI 21-cm Absorption Survey of Rich Abell Clusters
Radio-Optical Study of Double-Peaked AGNs: 3C 390.3
Astro Space Center of Lebedev Physical Institute, Moscow
Mareki Honma (NAOJ) On behalf of EATING VLBI collaboration
Radio Observations of Nearby HST BL Lacs
Dr. Jun Yang, Senior VLBI Support scientist
Compact radio jets and nuclear regions in galaxies
Presentation transcript:

Imaging nearby AGN at ultra high resolution with RadioAstron Tuomas Savolainen Aalto University Metsähovi Radio Observatory Max-Planck-Institut für Radioastronomie On behalf of the RadioAstron Nearby AGN Key Science Program team: J.Anderson, U.Bach, B.Boccardi, C.Casadio, G.Bruni, P.Edwards, J.Eilek, C.Fromm, G.Giovannini, M.Giroletti, K.Hada, P.Hardee, Y.Hagiwara, J.Hodgson, M.Honma, M.Kino, Y.Y.Kovalev, T.Krichbaum, A.Lobanov, S.S.Lee, D.Meier, M.Orienti, H.Nagai, S.O’Sullivan, C.Reynolds, B.W.Sohn, K.V.Sokolovsky, S.Tingay, J.A.Zensus

RadioAstron Nearby AGN KSP - Aims Near-perigee imaging observations of well-studied, nearby radio galaxies at 1.6, 5 and 22 GHz Target sources at distances of 4-75 Mpc  ultra-high spatial resolution (down to a few R S ) Study the structure and extent of the acceleration and collimation zone Study the onset of instabilities Search for compact substructure Multi-frequency observations for spectral and core-shift studies – Free-free absorption mapping at high resolution – Measuring magnetic fields from synchrotron self-absorption

Nearby AGN KSP Targets 0.83 x 0.68 mas Cen A (5 GHz VSOP) Horiuchi et al. (2006) (Nagai et al. 2014) 3C84 (43 GHz VLBA) Walker et al M87 (VLBA)

Nearby AGN KSP observations in AO-1 3C 84 5/22 GHz Sep 21 ’13 M87 5/22 GHz Feb 4 ’14 M GHz Jun 4 ’14 Cen A 5/22 GHz Feb 13 ’14 Cen A 22 GHz Mar 27 ’14 ~10 D Earth 30 ground stations 5 GHz correlated (Bonn) 33 ground stations correlation ongoing (Bonn) 30 ground stations not yet correlated (Bonn) 5 ground stations correlation ongoing (Curtin) ~11 D Earth ~6 D Earth ~4 D Earth 6 ground stations correlation ongoing (Curtin) EVN out-of-session observations Special thanks to the EVN and telescope schedulers (especially to Richard Porcas!), and to the JIVE support personel.

FIRST PRELIMINARY RESULTS: SPACE-VLBI IMAGE OF 3C84

3C84 at 5/22 GHz 5 GHz 22 GHz 5/22 GHz

3C84 at 5GHz Correlation with a modified DiFX at the MPIfR RadioAstron fringes were clearly detected (both in PIMA and AIPS): – Min. baseline length: 0.2ED (RA-KL, SNR 400) – Max. baseline length with a clear detection: 6.9ED (RA- EF, SNR 8.6) – Clear space-to-ground fringe detections in 24/47 scans RA-EF baseline of 6.9ED (1.4Gλ)

3C84 at 5GHz ground-only image

3C84 at 5GHz RadioAstron visibilities Green: Ground-ground baselines Black: Baselines to RadioAstron

3C84 at 5GHz with space baselines uvw 5,0; beam 1.18x0.10mas 0.8x0.4mas; Asada et al. 2006) 1 mas 3C84 (43 GHz VLBA) (Nagai et al. 2014) T b > 2x10 11 K C3 C2 “jet” Uvrange 0-700Mλ beam 0.9x0.5mas

3C84 at 5GHz with space baselines RA data and ground-only model RA data and ground+space model

3C84 - Other frequencies 5 GHz 1 mas 15 GHz Peak: 1.5 Jy/beam beam 0.9x0.5mas 43 GHz 5 GHz Core Peak: 5.3 Jy/beam beam 0.8x0.3mas Peak: 2.5 Jy/beam beam 0.4x0.15mas

3C84 - Spectra GHz spectral index GHz spectral index C1, C2 and C3 ALL have inverted spectrum at 5GHz C3 C2 C1

Summary 3C84, M87 and Cen A were observed within the RadioAstron Nearby AGN KSP at 1.6 (M87), 5 and 22GHz Correlation and data analysis are ongoing – the first fully correlated experiment GHz) resulted in fringe detections on space baselines up to 6.9 D Earth RadioAstron baselines contain significant structural information, but due to a pathological (u,v) coverage, imaging is challenging – direct modelling of the visibilities also needed Component C3 is the brightest one at 5 GHz (>2x10 11 K) All core region features have inverted spectra at 5 GHz  accurate T b measurement will give the magnetic flux density High expectations for the 22 GHz RadioAstron data

BACKUP SLIDES

3C84 at 5GHz - calibration accuracy of the SRT Green: Ground-ground baselines Black: RadioAstron-Kalyazin baseline (<1ED)

Nearby AGN KSP observations in AO-1 Sep : 3C84 – Baselines up to ~10 D Earth – 5/22GHz w/ SRT + 15/43GHz w/ VLBA+VLA; 5 GHz correlated (Bonn) – 26/30 scheduled ground stations produced data Feb 4/5 2014: M87 – Baselines up to ~11 D Earth – 5/22GHz w/ SRT + 15/43GHz w/ VLBA; correlation in progress (Bonn) – 28/33 scheduled ground stations produced data Feb : Cen A – Baselines up to ~6 D earth – 5 and 22 GHz w/ SRT; correlation in progress (Curtin) – 5 scheduled ground stations Mar : Cen A – Baselines up to ~4 D earth – 22 GHz w/ SRT; correlation in progress (Curtin) – 6 scheduled ground stations Jun 4/5 2014: M87 – Baselines up to ~6 D earth – 1.6 GHz w/SRT; not yet correlated (Bonn) – 30 scheduled ground stations incl. Sardinia

3C84 in the VSOP era VSOP observations by Asada et al. (2006): – Resolution of 0.78x0.39mas at 5GHz – Expansion and inner proper motions of southern radio lobe – Lobe age matches to 1959 outburst Asada et al. (2006)

3C84 at 5GHz - acceleration residuals Original orbit reconstruction A new reconstruction of the orbit using back-extrapolation 0.5 mHz/s ! mHz/s

3C84 at 5GHz Self-calibration and imaging First an image was made with ground telescopes only and this was used to self-calibrate GRT phase (10s) and amplitude (30s) Obtained GRT gain corrections applied to the full data set Multiple rounds of SRT phase self-cal with 60s solution interval Amplitude self-cal of the SRT (one solution for the whole observation) gave corrections <20%, not applied in the end Weighting is important: (super-)uniform with little or no weight based on vis. errors

Phase-cal solutions for RA (calib) SNR > 3No SNR cut-off

3C84 at 5GHz Amp. vs. (u,v) radius for ground data

Other restoring beam sizes 0.60x0.20mas 0.45x0.15mas

Other restoring beam sizes 0.30x0.10mas 0.50x0.50mas

Other restoring beam sizes 0.40x0.40mas 0.30x0.30mas

Effect of (u,v) weights uvw 2,-0.5uvw 2,0

Effect of (u,v) weights uvw 10,0uvw 5,0

JVLA fluxes WIDAR data as a by-product of phasing Unresolved core structure – 5GHz17.5 Jy – 15 GHz35.9 Jy – 22 GHz42.3 Jy – 43 GHz29.3 Jy