aleksandar shulevski + the nearby agn group (astron)
TRANSCRIPT
![Page 1: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/1.jpg)
Radiative age mapping of the B2 0924+30 relic using LOFAR
Aleksandar Shulevski + the nearby AGN group (ASTRON)
![Page 2: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/2.jpg)
OUTLINE:
• AGN radio relics
• A LOFAR look at the B2 0924+30 relicspectral and ageing analysis
• Results and prospects
![Page 3: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/3.jpg)
- Only observable tracer of past AGN activity
- Very few relics observed so farthat is about to change…
LOFAR - high spatial resolution below 200 MHzGood at imaging low surface brightness objects
AGN radio relics:
![Page 4: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/4.jpg)
Morphology: no jets, weak or no radio core (FR II case)
Way to ascertain the AGN duty cycle (Ton / Toff)
AGN radio relics:
radiative energy losses - steep high frequency spectra
studies over large bandwidth -essential for proper age characterisation
![Page 5: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/5.jpg)
Importance: Total energy / momentum deposited
over cosmic time in:
ISM - interrupt / quench star formationIGM - heating / cooling balance -
impact on structure formation
AGN radio relics:
© millenium
run
![Page 6: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/6.jpg)
B2 0924+30: relic at z=0.026host: elliptical galaxy brightest in a small group
22’’ LOFAR HBA - 140 MHz
![Page 7: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/7.jpg)
Integrated flux density:
CIoff model (Komissarov+ 94):
Toff = 93.5 +- 6.8 MyrTon = 54.5 +- 3.5 Myr
injection spectral index: -0.90 +- 0.07
B2 0924+30 LOFAR HBA
![Page 8: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/8.jpg)
140 - 600 MHzspectral index map
B2 0924+30
140 - 600 -1400 MHzspectral curvature map
JP model derivedradiative ages [Myr] - injection spectral index fixed to -0.9
LOFAR: high resolution at low frequencies
![Page 9: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/9.jpg)
B2 0924+30
LOFAR:science awaits
Abell 781
galactic merger (FR I)
double-double radio galaxy
B2 0924+30
28 MHz BWaround 140 MHz
60’’ x 43’’2.5 mJy/b rms noise
![Page 10: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/10.jpg)
More LOFAR relic discoveries:
The numbers are set to increasein the coming months
Brienza+ 2015
![Page 11: Aleksandar Shulevski + the nearby AGN group (ASTRON)](https://reader031.vdocuments.us/reader031/viewer/2022012015/615a62ef9d808248d950b199/html5/thumbnails/11.jpg)
- We can probe the low frequency spectra and use that additional spectral windowto put limits on the ages of resolved (nearby) sources.
- Due to the improved resolution at low frequencies, we can characterise the aged particle properties across the source. This allows us to investigate the activity historyand determine AGN duty cycles.
- Integrated spectra reflect the detailed properties of a source. Can be used astracers of activity out to higher redshifts for which current studies (using LOFAR)give a template.
Conclusions: