JWST meets Chandra: a large population of Compton thick, feedback-free, and intrinsically X-ray weak AGN, with a sprinkle of SNe
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866912152593367040 |
|---|---|
| author | Maiolino, Roberto Risaliti, Guido Signorini, Matilde Trefoloni, Bartolomeo Juodzbalis, Ignas Scholtz, Jan Uebler, Hannah D'Eugenio, Francesco Carniani, Stefano Fabian, Andy Ji, Xihan Mazzolari, Giovanni Bertola, Elena Brusa, Marcella Bunker, Andrew J. Charlot, Stephane Comastri, Andrea Cresci, Giovanni DeCoursey, Christa Noel Egami, Eiichi Fiore, Fabrizio Gilli, Roberto Perna, Michele Tacchella, Sandro Venturi, Giacomo |
| author_facet | Maiolino, Roberto Risaliti, Guido Signorini, Matilde Trefoloni, Bartolomeo Juodzbalis, Ignas Scholtz, Jan Uebler, Hannah D'Eugenio, Francesco Carniani, Stefano Fabian, Andy Ji, Xihan Mazzolari, Giovanni Bertola, Elena Brusa, Marcella Bunker, Andrew J. Charlot, Stephane Comastri, Andrea Cresci, Giovanni DeCoursey, Christa Noel Egami, Eiichi Fiore, Fabrizio Gilli, Roberto Perna, Michele Tacchella, Sandro Venturi, Giacomo |
| contents | We investigate the X-ray properties of a sample of 71 broad line and narrow line AGN at 2$<$z$<$11 discovered by JWST in the GOODS fields, which have the deepest Chandra observations ever obtained. Despite the widespread presence of AGN signatures in their rest-optical and -UV spectra, the vast majority of them is X-ray undetected. The stacked X-ray data of the non-detected sources also results in a non-detection. The upper limit on the X-ray emission for many of these AGN is one or even two orders of magnitude lower than expected from a standard AGN SED. X-ray absorption by clouds with large (Compton-thick) column density and low dust content, such as the Broad Line Region (BLR) clouds, can explain the X-ray weakness. In this scenario the BLR covering factor should be much larger than in low-z AGN or luminous quasars; this is supported by the larger equivalent width of the broad component of H$α$ in JWST-selected AGN. We also find that the JWST-discovered AGN lack prominent, fast outflows, suggesting that, in JWST-selected AGN, dense gas lingers in the nuclear region, resulting in large covering factors. We also note that a large fraction of JWST-selected AGN matches the definition of NLSy1, typically accreting at high rates and characterized by a steep X-ray spectrum -- this can further contribute to their observed weakness at high-z. Finally, we discuss that the broad Balmer lines used to identify type 1 AGN cannot be ascribed to Very Massive Stars or Supernovae, although we show that some of the faintest broad lines could potentially be associated with superluminous SNe. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_00504 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | JWST meets Chandra: a large population of Compton thick, feedback-free, and intrinsically X-ray weak AGN, with a sprinkle of SNe Maiolino, Roberto Risaliti, Guido Signorini, Matilde Trefoloni, Bartolomeo Juodzbalis, Ignas Scholtz, Jan Uebler, Hannah D'Eugenio, Francesco Carniani, Stefano Fabian, Andy Ji, Xihan Mazzolari, Giovanni Bertola, Elena Brusa, Marcella Bunker, Andrew J. Charlot, Stephane Comastri, Andrea Cresci, Giovanni DeCoursey, Christa Noel Egami, Eiichi Fiore, Fabrizio Gilli, Roberto Perna, Michele Tacchella, Sandro Venturi, Giacomo Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena We investigate the X-ray properties of a sample of 71 broad line and narrow line AGN at 2$<$z$<$11 discovered by JWST in the GOODS fields, which have the deepest Chandra observations ever obtained. Despite the widespread presence of AGN signatures in their rest-optical and -UV spectra, the vast majority of them is X-ray undetected. The stacked X-ray data of the non-detected sources also results in a non-detection. The upper limit on the X-ray emission for many of these AGN is one or even two orders of magnitude lower than expected from a standard AGN SED. X-ray absorption by clouds with large (Compton-thick) column density and low dust content, such as the Broad Line Region (BLR) clouds, can explain the X-ray weakness. In this scenario the BLR covering factor should be much larger than in low-z AGN or luminous quasars; this is supported by the larger equivalent width of the broad component of H$α$ in JWST-selected AGN. We also find that the JWST-discovered AGN lack prominent, fast outflows, suggesting that, in JWST-selected AGN, dense gas lingers in the nuclear region, resulting in large covering factors. We also note that a large fraction of JWST-selected AGN matches the definition of NLSy1, typically accreting at high rates and characterized by a steep X-ray spectrum -- this can further contribute to their observed weakness at high-z. Finally, we discuss that the broad Balmer lines used to identify type 1 AGN cannot be ascribed to Very Massive Stars or Supernovae, although we show that some of the faintest broad lines could potentially be associated with superluminous SNe. |
| title | JWST meets Chandra: a large population of Compton thick, feedback-free, and intrinsically X-ray weak AGN, with a sprinkle of SNe |
| topic | Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2405.00504 |