Using Time Domain Astronomy to Explore AGN Ann E. Wehrle Space Science Ins=tute Collaborators: Mark Gurwell, Svetlana Jorstad, Alan Marscher, Dirk Grupe Fermi LAT Team, NuSTAR Team GASP Collabora=on (Claudia Raiteri, Massimo Villata) and many others SMA: The First Decade of Discovery, Cambridge, MA, 9-‐10 June 2014 Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 1 •  New all-‐sky surveys -‐most variable objects -‐ AGN and exo=c types of stars (SNe, CVs, pulsars, etc.) Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 2 Radio Loud AGN Contain Rela=vis=c Jets-‐ Strongly Variable on Timescales of Days-‐Months Blazars-‐ looking directly down the jet Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 3 Fermi Blazars =SMA Calibrators Fermi LAT Team-‐ 5 year sky, two strong blazar ﬂares per month, duty cycles vary Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 4 Brightest AGN at 230 GHz 45+ papers by various groups M. Gurwell, CfA/SAO (see his poster) Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 5 Flaring AGN Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 6 What does variability tell us about AGN physics? 1.  Rise-‐fall: Physical scale ( mod. Doppler factors), shock condi=ons 2.  Time delays: rela=ve loca=ons 3.  Amplitude: (+ modelling) changes in magne=c ﬁeld, number of electrons and energy distribu=on, blob size, distance 4.  Brightness correlated with image changes: loca=on 5.  Monitoring: PSD of ﬂuctua=ons could be func=on(ac=vity level, jet, corona, disk); turbulence) A.  break =mescale implies physical scale; B.  relaxa=on =mescale implies “corporate memory” Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 7 AGN Jet Ques=ons 1.  What is the parsec-‐scale structure at various wavebands? 2.  What are the physical characteris=cs of the jet? 3.  Are all ﬂaring events the same? Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 8 Strategy #1 ::: 1.  Predetermined targets for dedicated study, olen mul=wavelength campaigns, or single-‐telescope monitoring for months to years (e.g., 3C279, Hayashida et al. 2012 ApJ 754, 117) è y g r e n E Inverse Synchrotron Compton Frequency è Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 9 Strategy #2 2.  Targets of Opportunity triggered by unusual behavior such as historical brightening (fading) or lack of iden=ﬁed counterpart, e.g., Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 10

Using Time Domain Astronomy to Explore AGN PDF

29 Pages

2014

18.08 MB

English

Checking for file health...

Preview Using Time Domain Astronomy to Explore AGN

Using Time Domain Astronomy to Explore AGN Ann E. Wehrle Space Science Ins=tute Collaborators: Mark Gurwell, Svetlana Jorstad, Alan Marscher, Dirk Grupe Fermi LAT Team, NuSTAR Team GASP Collabora=on (Claudia Raiteri, Massimo Villata) and many others SMA: The First Decade of Discovery, Cambridge, MA, 9-‐10 June 2014 Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 1 •  New all-‐sky surveys -‐most variable objects -‐ AGN and exo=c types of stars (SNe, CVs, pulsars, etc.) Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 2 Radio Loud AGN Contain Rela=vis=c Jets-‐ Strongly Variable on Timescales of Days-‐Months Blazars-‐ looking directly down the jet Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 3 Fermi Blazars =SMA Calibrators Fermi LAT Team-‐ 5 year sky, two strong blazar ﬂares per month, duty cycles vary Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 4 Brightest AGN at 230 GHz 45+ papers by various groups M. Gurwell, CfA/SAO (see his poster) Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 5 Flaring AGN Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 6 What does variability tell us about AGN physics? 1.  Rise-‐fall: Physical scale ( mod. Doppler factors), shock condi=ons 2.  Time delays: rela=ve loca=ons 3.  Amplitude: (+ modelling) changes in magne=c ﬁeld, number of electrons and energy distribu=on, blob size, distance 4.  Brightness correlated with image changes: loca=on 5.  Monitoring: PSD of ﬂuctua=ons could be func=on(ac=vity level, jet, corona, disk); turbulence) A.  break =mescale implies physical scale; B.  relaxa=on =mescale implies “corporate memory” Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 7 AGN Jet Ques=ons 1.  What is the parsec-‐scale structure at various wavebands? 2.  What are the physical characteris=cs of the jet? 3.  Are all ﬂaring events the same? Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 8 Strategy #1 ::: 1.  Predetermined targets for dedicated study, olen mul=wavelength campaigns, or single-‐telescope monitoring for months to years (e.g., 3C279, Hayashida et al. 2012 ApJ 754, 117) è y g r e n E Inverse Synchrotron Compton Frequency è Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 9 Strategy #2 2.  Targets of Opportunity triggered by unusual behavior such as historical brightening (fading) or lack of iden=ﬁed counterpart, e.g., Ann E. Wehrle, SMA: First Decade of Discovery, 9-‐10 June 2014 10

See more

The list of books you might like

Most books are stored in the elastic cloud where traffic is expensive. For this reason, we have a limit on daily download.