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Title: A Strong Radio Brightening At The Jet Base Of M 87 During The Elevated Very High Energy Gamma-Ray State In 2012

Abstract

We report our intensive, high-angular-resolution radio monitoring observations of the jet in M 87 with the VLBI Exploration of Radio Astrometry (VERA) and the European VLBI Network (EVN) from February 2011 to October 2012, together with contemporaneous high-energy (HE; 100 MeV< E <100 GeV) -ray light curves obtained by the Fermi Large Area Telescope (LAT). During this period (specifically from February 2012 to March 2012), an elevated level of the M 87 flux is reported at very-high-energy (VHE; E > 100 GeV) -rays by VERITAS. We detected a remarkable (up to ~70%) increase of the radio flux density from the unresolved jet base (radio core) with VERA at 22 and 43 GHz coincident with the VHE activity. Meanwhile, we confirmed with EVN at 5 GHz that the peculiar knot HST-1, which is an alternative favored -ray production site located at &120 pc from the nucleus, remained quiescent in terms of its flux density and structure. These results in the radio bands strongly suggest that the VHE -ray activity in 2012 originates in the jet base within 0.03 pc or 56 Schwarzschild radii (the VERA spatial resolution of 0.4 mas at 43 GHz) from the central supermassive black hole. We furthermore » conducted VERA astrometry for the M 87 core at six epochs during the flaring period, and detected core shifts between 22 and 43 GHz, a mean value of which is similar to that measured in the previous astrometric measurements. We also discovered a clear frequency-dependent evolution of the radio core flare at 43, 22 and 5 GHz; the radio flux density increased more rapidly at higher frequencies with a larger amplitude, and the light curves clearly showed a time-lag between the peaks at 22 and 43 GHz, the value of which is constrained to be within ~ 35 - 124 days. This indicates that a new radio-emitting component was created near the black hole in the period of the VHE event, and then propagated outward with progressively decreasing synchrotron opacity. By combining the obtained core shift and time-lag, we estimated an apparent speed of the newborn component propagating through the opaque region between the cores at 22 and 43 GHz. We derived a sub-luminal speed (less than ~0.2c) for this component. This value is significantly slower than the super-luminal (~1.1c) features that appeared from the core during the prominent VHE flaring event in 2008, suggesting that the stronger VHE activity can be associated with the production of the higher Lorentz factor jet in M 87.« less

Authors:
 [1];  [2];  [3];  [4]; ORCiD logo [2];  [5];  [6];  [7];  [8];  [9];  [10];  [11];  [12];  [2];  [6];  [12];  [7];  [13];  [14];  [15] more »;  [16] « less
+ Show Author Affiliations
  1. Istituto Nazionale di Astrofisica (INAF), Bologna (Italy); National Astronomical Observatory of Japan, Tokyo (Japan)
  2. Istituto Nazionale di Astrofisica (INAF), Bologna (Italy)
  3. Japan Aerospace Exploration Agency, Tsukuba (Japan); Korea Astronomy and Space Science Inst. (KASI), Daejeon (Korea)
  4. Istituto Nazionale di Astrofisica (INAF), Bologna (Italy); Univ. of Bologna (Italy)
  5. Naval Research Lab. (NRL), Washington, DC (United States)
  6. Washington Univ., St. Louis, MO (United States)
  7. National Astronomical Observatory of Japan, Tokyo (Japan)
  8. Japan Aerospace Exploration Agency, Tsukuba (Japan)
  9. National Astronomical Observatory of Japan, Tokyo (Japan); Univ. of Tokyo (Japan)
  10. National Astronomical Observatory of Japan, Tokyo (Japan); The Graduate Univ. for Advanced Sciences, Tokyo (Japan)
  11. The Graduate Univ. for Advanced Sciences, Tokyo (Japan)
  12. Spanish National Research Council (CSIC), Granada (Spain)
  13. National Astronomical Observatory of Japan, Tokyo (Japan); Japan Aerospace Exploration Agency, Tsukuba (Japan); Univ. of Tokyo (Japan)
  14. Univ. of Trento (Italy)
  15. Kagoshima Univ. (Japan)
  16. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org.:
USDOE
OSTI Identifier:
1356468
Grant/Contract Number:  
AC02-76SF00515
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal
Additional Journal Information:
Journal Volume: 788; Journal Issue: 2; Journal ID: ISSN 0004-637X
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Hada, K., Giroletti, M., Kino, M., Giovannini, G., D'Ammando, F., Cheung, C. C., Beilicke, M., Nagai, H., Doi, A., Akiyama, K., Honma, M., Niinuma, K., Casadio, C., Orienti, M., Krawczynski, H., Gómez, J. L., Sawada-Satoh, S., Koyama, S., Cesarini, A., Nakahara, S., and Gurwell, M. A. A Strong Radio Brightening At The Jet Base Of M 87 During The Elevated Very High Energy Gamma-Ray State In 2012. United States: N. p., 2014. Web. doi:10.1088/0004-637X/788/2/165.
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Hada, K., Giroletti, M., Kino, M., Giovannini, G., D'Ammando, F., Cheung, C. C., Beilicke, M., Nagai, H., Doi, A., Akiyama, K., Honma, M., Niinuma, K., Casadio, C., Orienti, M., Krawczynski, H., Gómez, J. L., Sawada-Satoh, S., Koyama, S., Cesarini, A., Nakahara, S., & Gurwell, M. A. A Strong Radio Brightening At The Jet Base Of M 87 During The Elevated Very High Energy Gamma-Ray State In 2012. United States. https://doi.org/10.1088/0004-637X/788/2/165
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Hada, K., Giroletti, M., Kino, M., Giovannini, G., D'Ammando, F., Cheung, C. C., Beilicke, M., Nagai, H., Doi, A., Akiyama, K., Honma, M., Niinuma, K., Casadio, C., Orienti, M., Krawczynski, H., Gómez, J. L., Sawada-Satoh, S., Koyama, S., Cesarini, A., Nakahara, S., and Gurwell, M. A. Wed . "A Strong Radio Brightening At The Jet Base Of M 87 During The Elevated Very High Energy Gamma-Ray State In 2012". United States. https://doi.org/10.1088/0004-637X/788/2/165. https://www.osti.gov/servlets/purl/1356468.
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@article{osti_1356468,
title = {A Strong Radio Brightening At The Jet Base Of M 87 During The Elevated Very High Energy Gamma-Ray State In 2012},
author = {Hada, K. and Giroletti, M. and Kino, M. and Giovannini, G. and D'Ammando, F. and Cheung, C. C. and Beilicke, M. and Nagai, H. and Doi, A. and Akiyama, K. and Honma, M. and Niinuma, K. and Casadio, C. and Orienti, M. and Krawczynski, H. and Gómez, J. L. and Sawada-Satoh, S. and Koyama, S. and Cesarini, A. and Nakahara, S. and Gurwell, M. A.},
abstractNote = {We report our intensive, high-angular-resolution radio monitoring observations of the jet in M 87 with the VLBI Exploration of Radio Astrometry (VERA) and the European VLBI Network (EVN) from February 2011 to October 2012, together with contemporaneous high-energy (HE; 100 MeV< E <100 GeV) -ray light curves obtained by the Fermi Large Area Telescope (LAT). During this period (specifically from February 2012 to March 2012), an elevated level of the M 87 flux is reported at very-high-energy (VHE; E > 100 GeV) -rays by VERITAS. We detected a remarkable (up to ~70%) increase of the radio flux density from the unresolved jet base (radio core) with VERA at 22 and 43 GHz coincident with the VHE activity. Meanwhile, we confirmed with EVN at 5 GHz that the peculiar knot HST-1, which is an alternative favored -ray production site located at &120 pc from the nucleus, remained quiescent in terms of its flux density and structure. These results in the radio bands strongly suggest that the VHE -ray activity in 2012 originates in the jet base within 0.03 pc or 56 Schwarzschild radii (the VERA spatial resolution of 0.4 mas at 43 GHz) from the central supermassive black hole. We further conducted VERA astrometry for the M 87 core at six epochs during the flaring period, and detected core shifts between 22 and 43 GHz, a mean value of which is similar to that measured in the previous astrometric measurements. We also discovered a clear frequency-dependent evolution of the radio core flare at 43, 22 and 5 GHz; the radio flux density increased more rapidly at higher frequencies with a larger amplitude, and the light curves clearly showed a time-lag between the peaks at 22 and 43 GHz, the value of which is constrained to be within ~ 35 - 124 days. This indicates that a new radio-emitting component was created near the black hole in the period of the VHE event, and then propagated outward with progressively decreasing synchrotron opacity. By combining the obtained core shift and time-lag, we estimated an apparent speed of the newborn component propagating through the opaque region between the cores at 22 and 43 GHz. We derived a sub-luminal speed (less than ~0.2c) for this component. This value is significantly slower than the super-luminal (~1.1c) features that appeared from the core during the prominent VHE flaring event in 2008, suggesting that the stronger VHE activity can be associated with the production of the higher Lorentz factor jet in M 87.},
doi = {10.1088/0004-637X/788/2/165},
journal = {The Astrophysical Journal},
number = 2,
volume = 788,
place = {United States},
year = {Wed Jun 04 00:00:00 EDT 2014},
month = {Wed Jun 04 00:00:00 EDT 2014}
}
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text, January 2012

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text, January 2005

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text, January 2007

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    journal, December 2018

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    • Publications of the Astronomical Society of Japan, Vol. 69, Issue 4
    • DOI: 10.1093/pasj/psx054

    The Structure and Dynamics of the Subparsec Jet in M87 Based on 50 VLBA Observations over 17 Years at 43 GHz
    journal, March 2018

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    Parabolic Jets from the Spinning Black Hole in M87
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