Optical spectroscopy of blazars for the Cherenkov Telescope Array
<i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray B...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Goldoni, Paolo [verfasserIn] Pita, S. [verfasserIn] Boisson, C. [verfasserIn] Max-Moerbeck, W. [verfasserIn] Kasai, E. [verfasserIn] Williams, D. A. [verfasserIn] D’Ammando, F. [verfasserIn] Navarro-Aranguiz, V. [verfasserIn] Backes, M. [verfasserIn] Almeida, U. Barres de [verfasserIn] Becerra-Gonzalez, J. [verfasserIn] Cotter, G. [verfasserIn] Hervet, O. [verfasserIn] Lenain, J.-P. [verfasserIn] Lindfors, E. [verfasserIn] Sol, H. [verfasserIn] Wagner, Stefan [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
15 June 2021 |
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| Anmerkung: |
Gesehen am 19.07.2022 |
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| Umfang: |
21 |
| Übergeordnetes Werk: |
Enthalten in: Astronomy and astrophysics - Les Ulis : EDP Sciences, 1969, 650(2021), Artikel-ID A106, Seite 1-21 |
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| Übergeordnetes Werk: |
volume:650 ; year:2021 ; elocationid:A106 ; pages:1-21 ; extent:21 |
| Links: |
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| DOI / URN: |
10.1051/0004-6361/202040090 |
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| Katalog-ID: |
1810862671 |
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| 245 | 1 | 0 | |a Optical spectroscopy of blazars for the Cherenkov Telescope Array |c P. Goldoni, S. Pita, C. Boisson, W. Max-Moerbeck, E. Kasai, D.A. Williams, F. D’Ammando, V. Navarro-Aranguiz, M. Backes, U. Barres de Almeida, J. Becerra-Gonzalez, G. Cotter, O. Hervet, J.-P. Lenain, E. Lindfors, H. Sol, and S. Wagner |
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| 520 | |a <i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. | ||
| 700 | 1 | |a Pita, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Boisson, C. |e verfasserin |4 aut | |
| 700 | 1 | |a Max-Moerbeck, W. |e verfasserin |4 aut | |
| 700 | 1 | |a Kasai, E. |e verfasserin |4 aut | |
| 700 | 1 | |a Williams, D. A. |e verfasserin |4 aut | |
| 700 | 1 | |a D’Ammando, F. |e verfasserin |4 aut | |
| 700 | 1 | |a Navarro-Aranguiz, V. |e verfasserin |4 aut | |
| 700 | 1 | |a Backes, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Almeida, U. Barres de |e verfasserin |4 aut | |
| 700 | 1 | |a Becerra-Gonzalez, J. |e verfasserin |4 aut | |
| 700 | 1 | |a Cotter, G. |e verfasserin |4 aut | |
| 700 | 1 | |a Hervet, O. |e verfasserin |4 aut | |
| 700 | 1 | |a Lenain, J.-P. |e verfasserin |4 aut | |
| 700 | 1 | |a Lindfors, E. |e verfasserin |4 aut | |
| 700 | 1 | |a Sol, H. |e verfasserin |4 aut | |
| 700 | 1 | |a Wagner, Stefan |e verfasserin |0 (DE-588)1034487728 |0 (DE-627)745635997 |0 (DE-576)38209123X |4 aut | |
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10.1051/0004-6361/202040090 doi (DE-627)1810862671 (DE-599)KXP1810862671 (OCoLC)1341464268 DE-627 ger DE-627 rda eng Goldoni, Paolo verfasserin (DE-588)1262948568 (DE-627)181086254X aut Optical spectroscopy of blazars for the Cherenkov Telescope Array P. Goldoni, S. Pita, C. Boisson, W. Max-Moerbeck, E. Kasai, D.A. Williams, F. D’Ammando, V. Navarro-Aranguiz, M. Backes, U. Barres de Almeida, J. Becerra-Gonzalez, G. Cotter, O. Hervet, J.-P. Lenain, E. Lindfors, H. Sol, and S. Wagner 15 June 2021 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 19.07.2022 <i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Pita, S. verfasserin aut Boisson, C. verfasserin aut Max-Moerbeck, W. verfasserin aut Kasai, E. verfasserin aut Williams, D. A. verfasserin aut D’Ammando, F. verfasserin aut Navarro-Aranguiz, V. verfasserin aut Backes, M. verfasserin aut Almeida, U. Barres de verfasserin aut Becerra-Gonzalez, J. verfasserin aut Cotter, G. verfasserin aut Hervet, O. verfasserin aut Lenain, J.-P. verfasserin aut Lindfors, E. verfasserin aut Sol, H. verfasserin aut Wagner, Stefan verfasserin (DE-588)1034487728 (DE-627)745635997 (DE-576)38209123X aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 650(2021), Artikel-ID A106, Seite 1-21 Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:650 year:2021 elocationid:A106 pages:1-21 extent:21 https://doi.org/10.1051/0004-6361/202040090 Verlag Resolving-System lizenzpflichtig Volltext https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 650 2021 A106 1-21 21 2013 01 DE-16-250 4170247159 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2403 01 DE-LFER 4190979538 00 --%%-- --%%-- n --%%-- l01 22-09-22 2403 01 DE-LFER https://doi.org/10.1051/0004-6361/202040090 2403 01 DE-LFER https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_17 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1452090963 Wagner, Stefan 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_17 |
| spelling |
10.1051/0004-6361/202040090 doi (DE-627)1810862671 (DE-599)KXP1810862671 (OCoLC)1341464268 DE-627 ger DE-627 rda eng Goldoni, Paolo verfasserin (DE-588)1262948568 (DE-627)181086254X aut Optical spectroscopy of blazars for the Cherenkov Telescope Array P. Goldoni, S. Pita, C. Boisson, W. Max-Moerbeck, E. Kasai, D.A. Williams, F. D’Ammando, V. Navarro-Aranguiz, M. Backes, U. Barres de Almeida, J. Becerra-Gonzalez, G. Cotter, O. Hervet, J.-P. Lenain, E. Lindfors, H. Sol, and S. Wagner 15 June 2021 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 19.07.2022 <i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Pita, S. verfasserin aut Boisson, C. verfasserin aut Max-Moerbeck, W. verfasserin aut Kasai, E. verfasserin aut Williams, D. A. verfasserin aut D’Ammando, F. verfasserin aut Navarro-Aranguiz, V. verfasserin aut Backes, M. verfasserin aut Almeida, U. Barres de verfasserin aut Becerra-Gonzalez, J. verfasserin aut Cotter, G. verfasserin aut Hervet, O. verfasserin aut Lenain, J.-P. verfasserin aut Lindfors, E. verfasserin aut Sol, H. verfasserin aut Wagner, Stefan verfasserin (DE-588)1034487728 (DE-627)745635997 (DE-576)38209123X aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 650(2021), Artikel-ID A106, Seite 1-21 Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:650 year:2021 elocationid:A106 pages:1-21 extent:21 https://doi.org/10.1051/0004-6361/202040090 Verlag Resolving-System lizenzpflichtig Volltext https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 650 2021 A106 1-21 21 2013 01 DE-16-250 4170247159 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2403 01 DE-LFER 4190979538 00 --%%-- --%%-- n --%%-- l01 22-09-22 2403 01 DE-LFER https://doi.org/10.1051/0004-6361/202040090 2403 01 DE-LFER https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_17 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1452090963 Wagner, Stefan 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_17 |
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10.1051/0004-6361/202040090 doi (DE-627)1810862671 (DE-599)KXP1810862671 (OCoLC)1341464268 DE-627 ger DE-627 rda eng Goldoni, Paolo verfasserin (DE-588)1262948568 (DE-627)181086254X aut Optical spectroscopy of blazars for the Cherenkov Telescope Array P. Goldoni, S. Pita, C. Boisson, W. Max-Moerbeck, E. Kasai, D.A. Williams, F. D’Ammando, V. Navarro-Aranguiz, M. Backes, U. Barres de Almeida, J. Becerra-Gonzalez, G. Cotter, O. Hervet, J.-P. Lenain, E. Lindfors, H. Sol, and S. Wagner 15 June 2021 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 19.07.2022 <i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Pita, S. verfasserin aut Boisson, C. verfasserin aut Max-Moerbeck, W. verfasserin aut Kasai, E. verfasserin aut Williams, D. A. verfasserin aut D’Ammando, F. verfasserin aut Navarro-Aranguiz, V. verfasserin aut Backes, M. verfasserin aut Almeida, U. Barres de verfasserin aut Becerra-Gonzalez, J. verfasserin aut Cotter, G. verfasserin aut Hervet, O. verfasserin aut Lenain, J.-P. verfasserin aut Lindfors, E. verfasserin aut Sol, H. verfasserin aut Wagner, Stefan verfasserin (DE-588)1034487728 (DE-627)745635997 (DE-576)38209123X aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 650(2021), Artikel-ID A106, Seite 1-21 Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:650 year:2021 elocationid:A106 pages:1-21 extent:21 https://doi.org/10.1051/0004-6361/202040090 Verlag Resolving-System lizenzpflichtig Volltext https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 650 2021 A106 1-21 21 2013 01 DE-16-250 4170247159 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2403 01 DE-LFER 4190979538 00 --%%-- --%%-- n --%%-- l01 22-09-22 2403 01 DE-LFER https://doi.org/10.1051/0004-6361/202040090 2403 01 DE-LFER https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_17 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1452090963 Wagner, Stefan 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_17 |
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10.1051/0004-6361/202040090 doi (DE-627)1810862671 (DE-599)KXP1810862671 (OCoLC)1341464268 DE-627 ger DE-627 rda eng Goldoni, Paolo verfasserin (DE-588)1262948568 (DE-627)181086254X aut Optical spectroscopy of blazars for the Cherenkov Telescope Array P. Goldoni, S. Pita, C. Boisson, W. Max-Moerbeck, E. Kasai, D.A. Williams, F. D’Ammando, V. Navarro-Aranguiz, M. Backes, U. Barres de Almeida, J. Becerra-Gonzalez, G. Cotter, O. Hervet, J.-P. Lenain, E. Lindfors, H. Sol, and S. Wagner 15 June 2021 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 19.07.2022 <i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Pita, S. verfasserin aut Boisson, C. verfasserin aut Max-Moerbeck, W. verfasserin aut Kasai, E. verfasserin aut Williams, D. A. verfasserin aut D’Ammando, F. verfasserin aut Navarro-Aranguiz, V. verfasserin aut Backes, M. verfasserin aut Almeida, U. Barres de verfasserin aut Becerra-Gonzalez, J. verfasserin aut Cotter, G. verfasserin aut Hervet, O. verfasserin aut Lenain, J.-P. verfasserin aut Lindfors, E. verfasserin aut Sol, H. verfasserin aut Wagner, Stefan verfasserin (DE-588)1034487728 (DE-627)745635997 (DE-576)38209123X aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 650(2021), Artikel-ID A106, Seite 1-21 Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:650 year:2021 elocationid:A106 pages:1-21 extent:21 https://doi.org/10.1051/0004-6361/202040090 Verlag Resolving-System lizenzpflichtig Volltext https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 650 2021 A106 1-21 21 2013 01 DE-16-250 4170247159 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2403 01 DE-LFER 4190979538 00 --%%-- --%%-- n --%%-- l01 22-09-22 2403 01 DE-LFER https://doi.org/10.1051/0004-6361/202040090 2403 01 DE-LFER https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_17 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1452090963 Wagner, Stefan 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_17 |
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10.1051/0004-6361/202040090 doi (DE-627)1810862671 (DE-599)KXP1810862671 (OCoLC)1341464268 DE-627 ger DE-627 rda eng Goldoni, Paolo verfasserin (DE-588)1262948568 (DE-627)181086254X aut Optical spectroscopy of blazars for the Cherenkov Telescope Array P. Goldoni, S. Pita, C. Boisson, W. Max-Moerbeck, E. Kasai, D.A. Williams, F. D’Ammando, V. Navarro-Aranguiz, M. Backes, U. Barres de Almeida, J. Becerra-Gonzalez, G. Cotter, O. Hervet, J.-P. Lenain, E. Lindfors, H. Sol, and S. Wagner 15 June 2021 21 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Gesehen am 19.07.2022 <i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Pita, S. verfasserin aut Boisson, C. verfasserin aut Max-Moerbeck, W. verfasserin aut Kasai, E. verfasserin aut Williams, D. A. verfasserin aut D’Ammando, F. verfasserin aut Navarro-Aranguiz, V. verfasserin aut Backes, M. verfasserin aut Almeida, U. Barres de verfasserin aut Becerra-Gonzalez, J. verfasserin aut Cotter, G. verfasserin aut Hervet, O. verfasserin aut Lenain, J.-P. verfasserin aut Lindfors, E. verfasserin aut Sol, H. verfasserin aut Wagner, Stefan verfasserin (DE-588)1034487728 (DE-627)745635997 (DE-576)38209123X aut Enthalten in Astronomy and astrophysics Les Ulis : EDP Sciences, 1969 650(2021), Artikel-ID A106, Seite 1-21 Online-Ressource (DE-627)253390222 (DE-600)1458466-9 (DE-576)072283351 1432-0746 nnns volume:650 year:2021 elocationid:A106 pages:1-21 extent:21 https://doi.org/10.1051/0004-6361/202040090 Verlag Resolving-System lizenzpflichtig Volltext https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html Verlag kostenfrei Volltext GBV_USEFLAG_U GBV_ILN_2013 ISIL_DE-16-250 SYSFLAG_1 GBV_KXP GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2006 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2190 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 GBV_ILN_2403 GBV_ILN_2403 ISIL_DE-LFER AR 650 2021 A106 1-21 21 2013 01 DE-16-250 4170247159 00 --%%-- --%%-- --%%-- --%%-- l01 19-07-22 2403 01 DE-LFER 4190979538 00 --%%-- --%%-- n --%%-- l01 22-09-22 2403 01 DE-LFER https://doi.org/10.1051/0004-6361/202040090 2403 01 DE-LFER https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html 2013 01 DE-16-250 00 s hd2021 2013 01 DE-16-250 01 s (DE-627)1410508463 wissenschaftlicher Artikel (Zeitschrift) 2013 01 DE-16-250 02 s per_17 2013 01 DE-16-250 03 s s_21 2013 01 DE-16-250 04 p (DE-627)1452090963 Wagner, Stefan 2013 01 DE-16-250 04 k (DE-627)1416733973 ZAH Landessternwarte 2013 01 DE-16-250 04 s (DE-627)1410501914 Verfasser 2013 01 DE-16-250 04 s pos_17 |
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Goldoni, S. Pita, C. Boisson, W. Max-Moerbeck, E. Kasai, D.A. Williams, F. D’Ammando, V. Navarro-Aranguiz, M. Backes, U. Barres de Almeida, J. Becerra-Gonzalez, G. Cotter, O. Hervet, J.-P. Lenain, E. Lindfors, H. Sol, and S. Wagner</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">15 June 2021</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">21</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="500" ind1=" " ind2=" "><subfield code="a">Gesehen am 19.07.2022</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a"><i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. 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optical spectroscopy of blazars for the cherenkov telescope array |
| title_auth |
Optical spectroscopy of blazars for the Cherenkov Telescope Array |
| abstract |
<i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Gesehen am 19.07.2022 |
| abstractGer |
<i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Gesehen am 19.07.2022 |
| abstract_unstemmed |
<i>Context.<i/> Blazars are the most numerous class of high-energy (HE; <i>E<i/> ∼ 50 MeV−100 GeV) and very high-energy (VHE; <i>E<i/> ∼ 100 GeV−10 TeV) gamma-ray emitters. Currently, a measured spectroscopic redshift is available for only about 50% of gamma-ray BL Lacertae objects (BL Lacs), mainly due to the difficulty in measuring reliable redshifts from their nearly featureless continuum-dominated optical spectra. The knowledge of the redshift is fundamental for understanding the emission from blazars, for population studies and also for indirect studies of the extragalactic background light and searches for Lorentz invariance violation and axion-like particles using blazars.<i>Aims.<i/> This paper is the first in a series of papers that aim to measure the redshift of a sample of blazars likely to be detected with the upcoming Cherenkov Telescope Array (CTA), a ground-based gamma-ray observatory.<i>Methods.<i/> Monte Carlo simulations were performed to select those hard spectrum gamma-ray blazars detected with the <i>Fermi<i/>-LAT telescope still lacking redshift measurements, but likely to be detected by CTA in 30 hours of observing time or less. Optical observing campaigns involving deep imaging and spectroscopic observations were organised to efficiently constrain their redshifts. We performed deep medium- to high-resolution spectroscopy of 19 blazar optical counterparts with the Keck II, SALT, and ESO NTT telescopes. We searched systematically for spectral features and, when possible, we estimated the contribution of the host galaxy to the total flux.<i>Results.<i/> We measured eleven firm spectroscopic redshifts with values ranging from 0.1116 to 0.482, one tentative redshift, three redshift lower limits including one at <i>z<i/> ≥ 0.449 and another at <i>z<i/> ≥ 0.868. Four BL Lacs show featureless spectra. Gesehen am 19.07.2022 |
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| title_short |
Optical spectroscopy of blazars for the Cherenkov Telescope Array |
| url |
https://doi.org/10.1051/0004-6361/202040090 https://www.aanda.org/articles/aa/abs/2021/06/aa40090-20/aa40090-20.html |
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Pita, S. Boisson, C. Max-Moerbeck, W. Kasai, E. Williams, D. A. D’Ammando, F. Navarro-Aranguiz, V. Backes, M. Almeida, U. Barres de Becerra-Gonzalez, J. Cotter, G. Hervet, O. Lenain, J.-P. Lindfors, E. Sol, H. Wagner, Stefan |
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Pita, S. Boisson, C. Max-Moerbeck, W. Kasai, E. Williams, D. A. D’Ammando, F. Navarro-Aranguiz, V. Backes, M. Almeida, U. Barres de Becerra-Gonzalez, J. Cotter, G. Hervet, O. Lenain, J.-P. Lindfors, E. Sol, H. Wagner, Stefan |
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