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Artículos de revistas sobre el tema "BL Lacertae objects"

Autor: Grafiati

Publicado: 4 de junio de 2021

Última modificación: 20 de febrero de 2023

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1

Britzen, S., A. Witzel, B. P. Gong, J. W. Zhang, G. Krishna, A. Goyal, M. F. Aller, H. D. Aller y J. A. Zensus. "Understanding BL Lacertae objects". Astronomy and Astrophysics 515 (junio de 2010): A105. http://dx.doi.org/10.1051/0004-6361/200913685.

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2

Sandrinelli, A., S. Covino, A. Treves, A. M. Holgado, A. Sesana, E. Lindfors y V. F. Ramazani. "Quasi-periodicities of BL Lacertae objects". Astronomy & Astrophysics 615 (julio de 2018): A118. http://dx.doi.org/10.1051/0004-6361/201732550.

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We review the reports of possible year-long quasi-periodicities of BL Lac objects in the γ-ray and optical bands, and present a homogeneous time analysis of the light curves of PKS2155−304, PG1553+113, and BL Lac. Based on results from a survey covering the entire Fermi γ-ray sky we have estimated the fraction of possible quasi-periodic BL Lac objects. We compared the cyclical behaviour in BL Lac objects with that derived from the search of possible optical periodicities in quasars, and find that at z ≲ 1 the cosmic density of quasi-periodic BL Lac objects is larger than that of quasi-periodic quasars. If the BL Lac quasi-periodicities were due to a supermassive binary black hole (SBBH) scenario, there could be a tension with the upper limits on the gravitational wave background measured by the pulsar timing array. The argument clearly indicates the difficulties of generally associating quasi-periodicities of BL Lac objects with SBBHs.

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3

Stocke, John T. "New Observations of BL Lacertae Objects". Symposium - International Astronomical Union 175 (1996): 385–88. http://dx.doi.org/10.1017/s0074180900081171.

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This contribution is divided into three parts: 1. A summary of mostly published work that describes the new type of BL Lac Objects discovered with X-ray satellites, “X-ray Bright BL Lacs (XBLs)”, and their relationship to the previously known “radio bright BL Lacs (RBLs).” Most (but not all?) of the differences between XBLs and RBLs are explicable using a “viewing angle” model in which the soft X-ray emission emanates into a much wider cone (23-30°) than the radio emission (8-10°). 2. New ROSAT PSPC soft X-ray observations are presented for complete samples of XBLs and RBLs which may explain the absence of luminous optical emission lines in BL Lacs. 3. A deep, subarcsec optical imaging survey of a large (50) sample of both XBLs and RBLs conducted at the Canada-France-Hawaii 3.6m Telescope (CFHT), whose purpose was to characterize the host galaxies and clustering environment of BL Lacs. This work defines more precisely the “parent population” of BL Lacs and identifies a small number of discrepant objects which may not be “beamed FR 1s”.

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4

Paggi, A., A. Cavaliere, V. Vittorini y M. Tavani. "Power for dry BL Lacertae objects". Astronomy & Astrophysics 508, n.º 3 (diciembre de 2009): L31—L34. http://dx.doi.org/10.1051/0004-6361/200913566.

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5

Wolter, Anna, Alessandro Caccianiga, Roberto della Ceca y Tommaso Maccacaro. "Luminosity functions of BL Lacertae objects". Astrophysical Journal 433 (septiembre de 1994): 29. http://dx.doi.org/10.1086/174622.

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6

Fan, Jun-Hui, Tong-Xu Hua, Yu-Hai Yuan, Yong-Xiang Wang, Yi Liu, Jiang-Bo Su, Yong-Wei Zhang, Jiang-He Yang y Yong Huang. "Radio Polarization of BL Lacertae Objects". Publications of the Astronomical Society of Japan 58, n.º 6 (25 de diciembre de 2006): 945–49. http://dx.doi.org/10.1093/pasj/58.6.945.

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7

Andruchow, I., G. E. Romero y S. A. Cellone. "Polarization microvariability of BL Lacertae objects". Astronomy & Astrophysics 442, n.º 1 (30 de septiembre de 2005): 97–107. http://dx.doi.org/10.1051/0004-6361:20053325.

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8

Sbarufatti, B., R. Falomo, A. Treves y J. Kotilainen. "Optical spectroscopy of BL Lacertae objects". Astronomy & Astrophysics 457, n.º 1 (12 de septiembre de 2006): 35–43. http://dx.doi.org/10.1051/0004-6361:20065455.

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9

Moles, M., J. M. Garcia-Pelayo, J. Masegosa y A. Aparicio. "UBVRI observations of BL Lacertae objects". Astrophysical Journal Supplement Series 58 (junio de 1985): 255. http://dx.doi.org/10.1086/191040.

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10

Sbarufatti, B., A. Treves y R. Falomo. "Imaging Redshifts of BL Lacertae Objects". Astrophysical Journal 635, n.º 1 (10 de diciembre de 2005): 173–79. http://dx.doi.org/10.1086/497022.

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11

Qin, Y. P. y G. Z. Xie. "Decijansky Radio Flux BL Lacertae Objects". Astrophysical Journal 487, n.º 1 (20 de septiembre de 1997): L41—L44. http://dx.doi.org/10.1086/310860.

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12

Lamer, G., H. Brunner y R. Staubert. "ROSAT Observations of Bright BL Lacertae Objects". Symposium - International Astronomical Union 159 (1994): 377. http://dx.doi.org/10.1017/s0074180900175692.

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We have compiled a sample of 23 X-ray and radio selected BL Lacertae objects which have been observed with the Position Sensitive Proportional Counter (PSPC) on board of the ROSAT Satellite. The sample consists of three parts:In Table I results from 4 objects observed for their known rapid X-ray variability are presented. 5 objects are the BL Lac subset of a complete sample of flat spectrum radio sources with 5 GHz flux densities > 1 Jy. Detailed results from this sample will be published in Brunner et al. 1993. The data of the 14 remainig objects were collected from the ROSAT data archive to supplement the sample. The whole sample contains 7 X-ray selected objects (XBLs,αOX < 1.2) and 16 radio selected objects (RBLs).The X-ray spectra of the sources are well described by single power laws with galactic absorption. The X-ray energy indices αX are widely dispersed around a mean of 1.34. Significant X-ray flux variability and correlated spectral variability was detected on timescales down to hours. The object H 1218+304 was found to be rapidly variable within each of three observations. Its spectral hardness is correlated with the flux level (see Table I).We calculated the intrinsic distributions of the spectral indices αX for the XBL and RBL samples and of the differences between ROSAT and EXOSAT ME spectral indices αPSPC – αME (only XBL sample) using a maximum likelihood fit. There is no significant difference in the mean spectral indices between the X-ray and radio selected subsamples. The mean values < αX > are 1.34 for XBLs and 1.33 for RBLs. The spectra of the X-ray selected objects slightly steepen at higher X-ray energies (< αPSPC – αME > = −0.11). This supports the view that the X-ray emission of XBLs is supplied by synchrotron radiation. The steepening of the X-ray spectrum is then due to a cutoff in the energy distribution of the electrons.

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13

Xie, G. Z., Y. H. Zhang, K. H. Li, F. K. Liu, J. C. Wang y X. M. Wang. "CCD Photometry of 12 BL Lacertae Objects". Astronomical Journal 111 (marzo de 1996): 1065. http://dx.doi.org/10.1086/117852.

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14

Xie, G. Z., S. B. Zhou, B. Z. Dai, E. W. Liang, K. H. Li, J. M. Bai, S. Y. Xing y W. W. Liu. "Photometric monitoring of 12 BL Lacertae objects". Monthly Notices of the Royal Astronomical Society 329, n.º 4 (febrero de 2002): 689–99. http://dx.doi.org/10.1046/j.1365-8711.2002.04952.x.

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15

Miller, H. R., M. T. Carini y B. D. Goodrich. "Detection of microvariability for BL Lacertae objects". Nature 337, n.º 6208 (febrero de 1989): 627–29. http://dx.doi.org/10.1038/337627a0.

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16

Zheng, Y. G., X. Zhang y X. W. Bi. "Optical Spectra of Four BL Lacertae Objects". Publications of the Astronomical Society of the Pacific 119, n.º 855 (mayo de 2007): 477–82. http://dx.doi.org/10.1086/519175.

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17

Cavaliere, A., E. Giallongo y F. Vagnetti. "BL Lacertae objects as an evolutionary population". Symposium - International Astronomical Union 119 (1986): 491–92. http://dx.doi.org/10.1017/s0074180900153252.

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If the BL Lac Objects are active nuclei with a beamed component that is dominant when directed at us, their observed luminosity function must comprise a flat faint branch: N(L)dL ∝ L1+1/pdL with p=4.5 (Urry and Shafer 1984). If this is flatter than the LF NP(L) of the parent objects at equal observed L, then we expect the counts of BL Lacs to flatten out in turn at fluxes quite higher than the counts of the parents, even when both populations evolve strongly and uniformly with comparable timescales (Cavaliere, Giallongo and Vagnetti 1985).

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18

Sol, Hélène y Lourdes Vicente. "A Tentative Sketch for BL Lacertae Objects". Symposium - International Astronomical Union 159 (1994): 473. http://dx.doi.org/10.1017/s0074180900176521.

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VLBI polarization data show magnetic field configuration parallel to the nuclear jet in quasars and perpendicular to it in BL Lac objects. It appears difficult to account for this contrast within the unified scheme for AGN. To investigate a direct explanation of this peculiarity of BL Lac objects, we study the possibilities of propagation and radiation of beams of particles in transverse ambient magnetic field. High energy streams with kinetic energy density larger than the ambient magnetic one, Ekin > Emag, can easily propagate with enhancement of the transverse magnetic field at the leading edge of the stream and reconnection of magnetic lines in its wake. Synchrotron radiation in front shocks naturally leads to the observed polarization. Moreover self-polarization, with formation of charge layers and E × B drift velocity, allows substantial propagation for even lower energy streams with Ekin < Emag, as long as their density no is large enough, typically κ = 4πnomic2/B2 > 1. Such low energy streams are non diamagnetic and do not modify the ambient field. Any high energy tail of the total particle distribution in the jet therefore radiates in the transverse field pattern. This concerns for instance the BL Lac object W Comae if we assume a proton-electron jet with bulk velocity vo = 0.1c (as the source does not require relativistic beaming so far), an equipartition magnetic field B = 0.02 G and a density of radiating particles nr = 0.05cm−3 at about 7 pc from the nucleus (knot K3). For nr/no = 10−3, one gets the stream density no = 50cm−3 which allows good propagation as κ reaches 2 × 103, and still corresponds to a moderate mass outflow of 0.06 M⊙ /year for a VLBI jet cross-sectional area of 2pc2.

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19

Smith, Paul S., G. Grant Williams, Gary D. Schmidt, Aleksandar M. Diamond‐Stanic y Dennis L. Means. "Highly Polarized Optically Selected BL Lacertae Objects". Astrophysical Journal 663, n.º 1 (julio de 2007): 118–24. http://dx.doi.org/10.1086/517992.

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20

Xie Guang-zhong, Hao Peng-jiu, Lu Ru-wei y Li Kai-hua. "Optical behaviour of four BL lacertae objects". Chinese Astronomy and Astrophysics 12, n.º 3 (septiembre de 1988): 197–204. http://dx.doi.org/10.1016/0275-1062(88)90047-1.

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21

Meisner, Aaron M. y Roger W. Romani. "IMAGING REDSHIFT ESTIMATES FOR BL LACERTAE OBJECTS". Astrophysical Journal 712, n.º 1 (24 de febrero de 2010): 14–25. http://dx.doi.org/10.1088/0004-637x/712/1/14.

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22

Cavaliere, A. y D. Malquori. "The Evolution of the BL Lacertae Objects". Astrophysical Journal 516, n.º 1 (1 de mayo de 1999): L9—L12. http://dx.doi.org/10.1086/311984.

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23

Fan, J. H., K. S. Cheng y L. Zhang. "Polarization and Variations of BL Lacertae Objects". Publications of the Astronomical Society of Japan 53, n.º 2 (25 de abril de 2001): 201–5. http://dx.doi.org/10.1093/pasj/53.2.201.

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24

Tramacere, A., P. Giommi, E. Massaro, M. Perri, R. Nesci, S. Colafrancesco, G. Tagliaferri et al. "SWIFT observations of TeV BL Lacertae objects". Astronomy & Astrophysics 467, n.º 2 (20 de febrero de 2007): 501–8. http://dx.doi.org/10.1051/0004-6361:20066226.

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25

Gabuzda, D. C., A. B. Pushkarev y T. V. Cawthorne. "3.6 cm VLBI Total Intensity and Polarization Images of BL Lacertae Objects". Symposium - International Astronomical Union 175 (1996): 51–52. http://dx.doi.org/10.1017/s0074180900079985.

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The major distinguishing features of BL Lacertae Objects are weak or absent line emission and strong and variable optical, infrared, and radio polarization (Angel and Stockman 1980; Kollgaard 1994). The radio emission and much of the optical emission is believed to be synchrotron radiation. There are now some 20 BL Lacertae objects for which VLBI polarization (VLBP) images have been made at λ = 6 cm (Gabuzda et al. 1994 and references therein). In nearly every BL Lacertae object in which polarization structure has been detected, the polarization position angles in knots in the jets are nearly parallel to the VLBI structural axis. Assuming the jet components to be optically thin, the magnetic fields inferred by this orientation are nearly perpendicular to the direction of the jet; perhaps the most natural interpretation of this is that the knots are associated with shocks that compress an initially tangled magnetic field as they propagate down the VLBI jet, enhancing the magnetic field transverse to the compression (Laing 1980; Hughes, Aller, & Aller 1989).

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26

Padovani, Paolo y Paolo Giommi. "The Rosat X-Ray Spectra of BL Lacertae Objects". Symposium - International Astronomical Union 175 (1996): 267–68. http://dx.doi.org/10.1017/s0074180900080761.

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We have analyzed the X-ray spectra of all BL Lacs observed (as pointed or serendipitous sources) by ROSAT. Spectral indices were obtained from the hardness ratios given in the WGA catalogue, a large list of X-ray sources generated from all the ROSAT PSPC pointed observations. The selection of the objects was done by cross-correlating the first revision of the WGA catalogue with our recent catalogue of BL Lacs. This resulted in 163 observations of 85 distinct BL Lacs, which correspond to about half the confirmed BL Lacs presently known. This represents the largest number of BL Lacs for which homogeneous X-ray spectral information is available and the largest BL Lac sample ever studied at X-ray frequencies.

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27

D'Amicis, R., R. Nesci, E. Massaro, M. Maesano, F. Montagni y F. D'Alessio. "Spectral Variability of BL Lac Objects". Publications of the Astronomical Society of Australia 19, n.º 1 (2002): 111–13. http://dx.doi.org/10.1071/as01113.

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AbstractWe present the relation between optical luminosity and spectral slope for eight BL Lac objects (3C66A, PKS 0422+00, S5 0716+71, OJ 287, ON 231, OQ 530, S5 1803+78 and BL Lacertae), derived from B, V, R, and I observations spanning a time interval of about 5 years. Four objects show a marked correlation between spectral slope and luminosity, being bluer when brighter, while for the other four the correlation is weaker or absent. Possible explanations are briefly discussed in the framework of current models of the BL Lac phenomenon.

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28

Landoni, Marco, R. Falomo, S. Paiano y A. Treves. "ZBLLAC: A Spectroscopic Database of BL Lacertae Objects". Astrophysical Journal Supplement Series 250, n.º 2 (15 de octubre de 2020): 37. http://dx.doi.org/10.3847/1538-4365/abb5ae.

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29

Padovani, P. y P. Giommi. "A Sample-oriented catalogue of BL Lacertae objects". Monthly Notices of the Royal Astronomical Society 277, n.º 4 (15 de diciembre de 1995): 1477–90. http://dx.doi.org/10.1093/mnras/277.4.1477.

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30

Smith, Eric P., C. P. O'Dea y S. A. Baum. "The megaparsec-scale environments of BL Lacertae objects". Astrophysical Journal 441 (marzo de 1995): 113. http://dx.doi.org/10.1086/175340.

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31

Hardcastle, M. J., D. M. Worrall, M. Birkinshaw y C. M. Canosa. "Unifying B2 radio galaxies with BL Lacertae objects". Monthly Notices of the Royal Astronomical Society 338, n.º 1 (1 de enero de 2003): 176–88. http://dx.doi.org/10.1046/j.1365-8711.2003.06039.x.

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32

Padovani, Paolo, Luigi Costamante, Paolo Giommi, Gabriele Ghisellini, Andrea Comastri, Anna Wolter, Laura Maraschi, Gianpiero Tagliaferri y C. Megan Urry. "BeppoSAXobservations of 1-Jy BL Lacertae objects - I". Monthly Notices of the Royal Astronomical Society 328, n.º 3 (diciembre de 2001): 931–43. http://dx.doi.org/10.1046/j.1365-8711.2001.04918.x.

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33

Laurent‐Muehleisen, S. A., R. I. Kollgaard, E. D. Feigelson, W. Brinkmann y J. Siebert. "The RGB Sample of Intermediate BL Lacertae Objects". Astrophysical Journal 525, n.º 1 (noviembre de 1999): 127–43. http://dx.doi.org/10.1086/307881.

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34

Tomaschitz, R. "Tachyonic γ-ray cascades from BL Lacertae objects". EPL (Europhysics Letters) 85, n.º 2 (enero de 2009): 29001. http://dx.doi.org/10.1209/0295-5075/85/29001.

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35

Landoni, M., R. Falomo, A. Treves y B. Sbarufatti. "Spectroscopy of BL Lacertae objects of extraordinary luminosity". Astronomy & Astrophysics 570 (octubre de 2014): A126. http://dx.doi.org/10.1051/0004-6361/201424232.

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36

Capetti, A. y C. M. Raiteri. "Looking for the least luminous BL Lacertae objects". Astronomy & Astrophysics 580 (agosto de 2015): A73. http://dx.doi.org/10.1051/0004-6361/201525890.

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37

Fan, J. H., G. Z. Xie, J. J. Li, J. Liu, S. L. Wen, R. R. Huang, Z. M. Tang y Y. J. Wang. "Radio-selected BL Lacertae objects and some correlations". Astrophysical Journal 415 (septiembre de 1993): 113. http://dx.doi.org/10.1086/173148.

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38

Horan, D. "VHE observations of BL Lacertae objects: 1995–2000". New Astronomy Reviews 48, n.º 5-6 (abril de 2004): 391–93. http://dx.doi.org/10.1016/j.newar.2003.12.016.

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39

Cassaro, P., C. Stanghellini, D. Dallacasa, M. Bondi y R. A. Zappalà. "Bendings of radio jets in BL Lacertae objects". Astronomy & Astrophysics 381, n.º 2 (enero de 2002): 378–88. http://dx.doi.org/10.1051/0004-6361:20011460.

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40

Kidger, Mark R. "CCD monitoring of quasars and BL Lacertae objects". Publications of the Astronomical Society of the Pacific 100 (octubre de 1988): 1248. http://dx.doi.org/10.1086/132311.

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41

Falomo, Renato, Jorge Melnick y Enrico G. Tanzi. "On the close environment of BL Lacertae objects". Nature 345, n.º 6277 (junio de 1990): 692–94. http://dx.doi.org/10.1038/345692a0.

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42

Rector, Travis A., John T. Stocke y Eric S. Perlman. "A Search for Low‐Luminosity BL Lacertae Objects". Astrophysical Journal 516, n.º 1 (mayo de 1999): 145–62. http://dx.doi.org/10.1086/307076.

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43

Padovani, Paolo, Paolo Giommi, Andrea Comastri, Gabriele Ghisellini, Tommaso Maccacaro, Franco Mantovani, Laura Maraschi et al. "BeppoSAX observations of 1 Jy BL lacertae objects". Nuclear Physics B - Proceedings Supplements 69, n.º 1-3 (enero de 1999): 431–34. http://dx.doi.org/10.1016/s0920-5632(98)00256-4.

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44

Gabuzda, D. C., D. H. Roberts, J. F. C. Wardle y L. F. Brown. "Milliarcsecond Polarization Properties of Several BL Lacertae Objects". Symposium - International Astronomical Union 129 (1988): 167–68. http://dx.doi.org/10.1017/s0074180900134400.

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We discuss the λ6 cm total intensity and polarization structures of a number of BL Lacertae objects at milliarcsecond resolution. 0235+164 was unresolved and weakly polarized at each of two epochs a year apart; each of the other objects displays structure in polarized flux. 0735+178 and 1749+096 can be adequately modeled by two or three point components—a “core” plus one or two “knots.” The core components were moderately polarized (≃ 5%), while “knots” may be polarized at 8% or more, consistent with these components being optically thin. Preliminary results for BL Lac indicate that the total intensity structure can be modeled well by a set of four gaussian components; the polarization structure is complex, but is dominated by the northernmost knot in the jet.

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45

Fan, J. H. y R. G. Lin. "Infrared Variation of Radio‐selected BL Lacertae Objects". Astrophysical Journal Supplement Series 121, n.º 1 (marzo de 1999): 131–57. http://dx.doi.org/10.1086/313191.

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46

Stocke, John T., Simon L. Morris, Isabella Gioia, Tommaso Maccacaro, R. E. Schild y A. Wolter. "No evidence for radio-quiet BL Lacertae objects". Astrophysical Journal 348 (enero de 1990): 141. http://dx.doi.org/10.1086/168221.

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47

Urry, C. M., R. F. Mushotzky y S. S. Holt. "X-ray spectroscopy of five BL Lacertae objects". Astrophysical Journal 305 (junio de 1986): 369. http://dx.doi.org/10.1086/164254.

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48

Romanishin, W. "Imaging redshift estimates for two BL Lacertae objects". Astrophysical Journal 320 (septiembre de 1987): 586. http://dx.doi.org/10.1086/165576.

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49

Hovatta, T., E. Lindfors, D. Blinov, V. Pavlidou, K. Nilsson, S. Kiehlmann, E. Angelakis et al. "Optical polarization of high-energy BL Lacertae objects". Astronomy & Astrophysics 596 (diciembre de 2016): A78. http://dx.doi.org/10.1051/0004-6361/201628974.

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50

Caccianiga, A., T. Maccacaro, A. Wolter, R. Della Ceca y I. M. Gioia. "On the Cosmological Evolution of BL Lacertae Objects". Astrophysical Journal 566, n.º 1 (10 de febrero de 2002): 181–86. http://dx.doi.org/10.1086/338073.

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