Spectropolarimetric view of the gamma-ray emitting NLS1 1H0323 + 342

Author:

Jose Jincen12,Rakshit Suvendu1ORCID,Panda Swayamtrupta34,Woo Jong-Hak5,Stalin C S6ORCID,Neha Sharma1,Pandey Shivangi17

Affiliation:

1. Aryabhatta Research Institute of Observational Sciences (ARIES) , Manora Peak, Nainital 263002 , India

2. Center for Basic Sciences, Pt. Ravishankar Shukla University , Raipur, Chhattisgarh 492010 , India

3. Laboratório Nacional de Astrofísica – MCTI , R. dos Estados Unidos, 154 - Nações, Itajubá, MG 37504-364 , Brazil

4. International Gemini Observatory/NSF NOIRLab , Casilla 603, La Serena , Chile

5. Department of Physics & Astronomy, Seoul National University , Seoul 08826 , Republic of Korea

6. Indian Institute of Astrophysics , Block II, Koramangala, Bangalore 560034 , India

7. Department of Applied Physics/Physics, M.J.P. Rohilkhand University , Bareilly, Uttar Pradesh 24300 , India

Abstract

ABSTRACT The gamma-ray emitting narrow-line Seyfert 1 galaxies are a unique class of objects that launch powerful jets from relatively lower-mass black hole systems compared to the Blazars. However, the black hole masses estimated from the total flux spectrum suffer from the projection effect, making the mass measurement highly uncertain. The polarized spectrum provides a unique view of the central engine through scattered light. We performed spectropolarimetric observations of the gamma-ray emitting narrow-line Seyfert 1 galaxy 1H0323 + 342 using SPOL/MMT. The degree of polarization and polarization angle are 0.122 $\pm$ 0.040 per cent and 142 $\pm$ 9 degrees, while the H $\alpha$ line is polarized at 0.265 $\pm$ 0.280 per cent. We decomposed the total flux spectrum and estimated broad H $\alpha$ full width at half maximum of 1015 km s$^{-1}$. The polarized flux spectrum shows a broadening similar to the total flux spectrum, with a broadening ratio of 1.22. The Monte Carlo radiative transfer code ‘STOKES’ applied to the data provides the best fit for a small viewing angle of 9–24 deg and a small optical depth ratio between the polar and the equatorial scatters. A thick broad-line region with significant scale height can explain a similar broadening of the polarized spectrum compared to the total flux spectrum with a small viewing angle.

Funder

SERB

DST

Conselho Nacional de Desenvolvimento Científico e Tecnológico

National Science Foundation

University of Arizona

Publisher

Oxford University Press (OUP)

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