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| Main Authors: | , , , , , , |
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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2505.14025 |
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| _version_ | 1866912383112314880 |
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| author | Pang, Yuxuan Wu, Xue-Bing Fu, Yuming Zhu, Rui Ji, Tao Ma, Qinchun Feng, Xiaotong |
| author_facet | Pang, Yuxuan Wu, Xue-Bing Fu, Yuming Zhu, Rui Ji, Tao Ma, Qinchun Feng, Xiaotong |
| contents | Slitless spectroscopy is a traditional method for selecting quasars. In this paper, we develop a procedure for selecting quasars (QSOs) using the 3D-HST G141 slitless spectra. We initially identify over 6,000 sources with emission lines broader than those typically found in emission line galaxies (ELGs) by analyzing the 1D spectra. These ``broad'' emission lines may originate from actual QSO broad lines ($\rm FWHM\geq1200~\rm km/s$) or the convolved narrow lines ($\rm FWHM = 200\sim 300\rm km/s$) in ELGs with effective radii $\geq$0.3" (2.5Kpc at z=1). We then propose a criterion based on the reliability of the QSO component in the forward modeling results. Using the known QSOs, ELGs, and simulation spectra, we find that our criterion successfully selects about 90\% of known QSOs with H$α$ or H$β$ line detection and point-like structures, with an ELG contamination rate of about 5\%. We apply this method to emission line sources without significant contamination and select 19 QSO candidates at redshift $z=0.12-1.56$. 12 of these candidates have Chandra X-ray detections. This sample covers a broader range of the rest-frame UV colors and has redder optical slopes compared to the SDSS QSOs, yet it is more likely to be composed of normal QSOs rather than little red dots. Through spectral analysis, the estimated black hole masses of the sample are $10^{6.9}-10^{8.3} M_{\odot}$. Our new candidates improve the completeness of the QSO sample at $z=0.8-1.6$ in the 3D-HST field. The proposed method will also be helpful for QSO selections via slitless spectroscopy in Euclid and the Chinese Space Station Telescope. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_14025 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Quasar identifications from the slitless spectra: a test from 3D-HST Pang, Yuxuan Wu, Xue-Bing Fu, Yuming Zhu, Rui Ji, Tao Ma, Qinchun Feng, Xiaotong Astrophysics of Galaxies Slitless spectroscopy is a traditional method for selecting quasars. In this paper, we develop a procedure for selecting quasars (QSOs) using the 3D-HST G141 slitless spectra. We initially identify over 6,000 sources with emission lines broader than those typically found in emission line galaxies (ELGs) by analyzing the 1D spectra. These ``broad'' emission lines may originate from actual QSO broad lines ($\rm FWHM\geq1200~\rm km/s$) or the convolved narrow lines ($\rm FWHM = 200\sim 300\rm km/s$) in ELGs with effective radii $\geq$0.3" (2.5Kpc at z=1). We then propose a criterion based on the reliability of the QSO component in the forward modeling results. Using the known QSOs, ELGs, and simulation spectra, we find that our criterion successfully selects about 90\% of known QSOs with H$α$ or H$β$ line detection and point-like structures, with an ELG contamination rate of about 5\%. We apply this method to emission line sources without significant contamination and select 19 QSO candidates at redshift $z=0.12-1.56$. 12 of these candidates have Chandra X-ray detections. This sample covers a broader range of the rest-frame UV colors and has redder optical slopes compared to the SDSS QSOs, yet it is more likely to be composed of normal QSOs rather than little red dots. Through spectral analysis, the estimated black hole masses of the sample are $10^{6.9}-10^{8.3} M_{\odot}$. Our new candidates improve the completeness of the QSO sample at $z=0.8-1.6$ in the 3D-HST field. The proposed method will also be helpful for QSO selections via slitless spectroscopy in Euclid and the Chinese Space Station Telescope. |
| title | Quasar identifications from the slitless spectra: a test from 3D-HST |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2505.14025 |