RADIO-WEAK BL LAC OBJECTS in the FERMI ERA

F. Massaro, E. J. Marchesini, R. D'Abrusco, N. Masetti, I. Andruchow, Howard A. Smith

Resultado de la investigación: Article

12 Citas (Scopus)

Resumen

The existence of "radio-weak BL Lac objects" (RWBLs) has been an open question, and has remained unsolved since the discovery that quasars could be radio-quiet or radio-loud. Recently, several groups identified RWBL candidates, mostly found while searching for low-energy counterparts of the unidentified or unassociated gamma-ray sources listed in the Fermi catalogs. Confirming RWBLs is a challenging task since they could be confused with white dwarfs (WDs) or weak emission line quasars (WELQs) when there are not sufficient data to precisely draw their broadband spectral energy distribution, and their classification is mainly based on a featureless optical spectra. Motivated by the recent discovery that Fermi BL Lacs appear to have very peculiar mid-IR emission, we show that it is possible to distinguish between WDs, WELQs, and BL Lacs using the [3.4]-[4.6]-[12] μm color-color plot built using the WISE magnitudes when the optical spectrum is available. On the basis of this analysis, we identify WISE J064459.38+603131 and WISE J141046.00+740511.2 as the first two genuine RWBLs, both potentially associated with Fermi sources. Finally, to strengthen our identification of these objects as true RWBLs, we present multifrequency observations for these two candidates to show that their spectral behavior is indeed consistent with that of the BL Lac population.

Idioma originalEnglish
Número de artículo113
PublicaciónAstrophysical Journal
Volumen834
N.º2
DOI
EstadoPublished - 10 ene 2017
Publicado de forma externa

Huella dactilar

Wide-field Infrared Survey Explorer
quasars
radio
optical spectrum
color
spectral energy distribution
catalogs
plots
broadband
energy

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Massaro, F., Marchesini, E. J., D'Abrusco, R., Masetti, N., Andruchow, I., & Smith, H. A. (2017). RADIO-WEAK BL LAC OBJECTS in the FERMI ERA. Astrophysical Journal, 834(2), [113]. https://doi.org/10.3847/1538-4357/834/2/113
Massaro, F. ; Marchesini, E. J. ; D'Abrusco, R. ; Masetti, N. ; Andruchow, I. ; Smith, Howard A. / RADIO-WEAK BL LAC OBJECTS in the FERMI ERA. En: Astrophysical Journal. 2017 ; Vol. 834, N.º 2.
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Massaro, F, Marchesini, EJ, D'Abrusco, R, Masetti, N, Andruchow, I & Smith, HA 2017, 'RADIO-WEAK BL LAC OBJECTS in the FERMI ERA', Astrophysical Journal, vol. 834, n.º 2, 113. https://doi.org/10.3847/1538-4357/834/2/113

RADIO-WEAK BL LAC OBJECTS in the FERMI ERA. / Massaro, F.; Marchesini, E. J.; D'Abrusco, R.; Masetti, N.; Andruchow, I.; Smith, Howard A.

En: Astrophysical Journal, Vol. 834, N.º 2, 113, 10.01.2017.

Resultado de la investigación: Article

TY - JOUR

T1 - RADIO-WEAK BL LAC OBJECTS in the FERMI ERA

AU - Massaro, F.

AU - Marchesini, E. J.

AU - D'Abrusco, R.

AU - Masetti, N.

AU - Andruchow, I.

AU - Smith, Howard A.

PY - 2017/1/10

Y1 - 2017/1/10

N2 - The existence of "radio-weak BL Lac objects" (RWBLs) has been an open question, and has remained unsolved since the discovery that quasars could be radio-quiet or radio-loud. Recently, several groups identified RWBL candidates, mostly found while searching for low-energy counterparts of the unidentified or unassociated gamma-ray sources listed in the Fermi catalogs. Confirming RWBLs is a challenging task since they could be confused with white dwarfs (WDs) or weak emission line quasars (WELQs) when there are not sufficient data to precisely draw their broadband spectral energy distribution, and their classification is mainly based on a featureless optical spectra. Motivated by the recent discovery that Fermi BL Lacs appear to have very peculiar mid-IR emission, we show that it is possible to distinguish between WDs, WELQs, and BL Lacs using the [3.4]-[4.6]-[12] μm color-color plot built using the WISE magnitudes when the optical spectrum is available. On the basis of this analysis, we identify WISE J064459.38+603131 and WISE J141046.00+740511.2 as the first two genuine RWBLs, both potentially associated with Fermi sources. Finally, to strengthen our identification of these objects as true RWBLs, we present multifrequency observations for these two candidates to show that their spectral behavior is indeed consistent with that of the BL Lac population.

AB - The existence of "radio-weak BL Lac objects" (RWBLs) has been an open question, and has remained unsolved since the discovery that quasars could be radio-quiet or radio-loud. Recently, several groups identified RWBL candidates, mostly found while searching for low-energy counterparts of the unidentified or unassociated gamma-ray sources listed in the Fermi catalogs. Confirming RWBLs is a challenging task since they could be confused with white dwarfs (WDs) or weak emission line quasars (WELQs) when there are not sufficient data to precisely draw their broadband spectral energy distribution, and their classification is mainly based on a featureless optical spectra. Motivated by the recent discovery that Fermi BL Lacs appear to have very peculiar mid-IR emission, we show that it is possible to distinguish between WDs, WELQs, and BL Lacs using the [3.4]-[4.6]-[12] μm color-color plot built using the WISE magnitudes when the optical spectrum is available. On the basis of this analysis, we identify WISE J064459.38+603131 and WISE J141046.00+740511.2 as the first two genuine RWBLs, both potentially associated with Fermi sources. Finally, to strengthen our identification of these objects as true RWBLs, we present multifrequency observations for these two candidates to show that their spectral behavior is indeed consistent with that of the BL Lac population.

KW - BL Lacertae objects: general

KW - galaxies: active

KW - quasars: emission lines

KW - quasars: general

KW - radiation mechanisms: non-thermal

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JF - Astrophysical Journal

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Massaro F, Marchesini EJ, D'Abrusco R, Masetti N, Andruchow I, Smith HA. RADIO-WEAK BL LAC OBJECTS in the FERMI ERA. Astrophysical Journal. 2017 ene 10;834(2). 113. https://doi.org/10.3847/1538-4357/834/2/113