The Mid‐Infrared Emission of M87

Perlman, Eric S.; Mason, Rachel; Packham, C.; Levenson, N. A.; Elitzur, Moshe; Schaefer, J. J.; Imanishi, Masatoshi; Sparks, W. B.; Radomski, J. T.

doi:10.1086/518781

Cited by 60 publications

(75 citation statements)

References 58 publications

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“…We recall that M 87 is a LINER. Apart from the thermal component of its mid-infrared emission, we also observe its power law synchrotron-like emission of similar intensity 10 39 erg/s (Perlman et al 2007). The thermal component of temperature 50 K is the radiation of the dust around the central energy source.…”

Section: Discussionmentioning

confidence: 68%

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Low-luminosity AGNs

Istomin

Sol

2011

A&A

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Context. We propose that low-luminosity AGNs (LLAGNs), or some of them, are sources extracting their energy from the black hole rotation by the Blandford-Znajek mechanism. Aims. It is shown that almost all energy of the black hole rotation is converted to relativistic protons in a jet. Owing to the high magnetic-field magnitude near the black hole, required for the Blandford-Znajek mechanism, electrons are not strongly accelerated because of their high synchrotron losses. Conversely, protons gain energies on the order of (10 4 −10 5 )m p c 2 when crossing the light cylinder surface. Protons are also accelerated in a disk by 2D turbulent motion of the disk matter. Methods. We calculate the luminosity of the synchrotron radiation by fast protons in the disk, the frequencies of this radiation being in the infrared band, and the luminosities corresponding to LLAGNs. We measure the very high energy (VHE) radiation luminosities from the disk and the jet, finding that VHE radiation is produced by collisions of accelerated protons with surrounding matter. Results. We predict a correlation between the infrared luminosity L IR and the VHE luminosityIR M 3/2 , where M is the mass of a black hole. Two low-luminosity sources Sgr A* and M 87, for which luminosities L IR and L VHE are known, appear to follow this scheme. Conclusions. The discovery of new bright VHE sources from LLAGNs could confirm our hypotheses that they are energy sources powered by the Blandford-Znajek mechanism.

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Section: Discussionmentioning

confidence: 68%

“…For Sgr A*, we have L VHE = 3 × 10 34 erg/s (Aharonian et al 2009a) and L s = L IR = 10 36 erg/s (Yuan et al 2003), M = 3.6 × 10 6 M , and for M 87 L VHE = 3 × 10 40 erg/s and L s = L IR = 10 39 erg/s (Perlman et al 2007), M = 3 × 10 9 M . Substituting these values in to Eq.…”

Section: Discussionmentioning

confidence: 93%

Low-luminosity AGNs

Istomin

Sol

2011

A&A

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“…Therefore, in the light of the current results, we will discuss probable mechanisms responsible for the observed and possibly intrinsic differences. There is strong evidence that the dusty obscuring torus in low luminosity AGN is absent or is thinner than expected in higher luminosities (e.g., Whysong & Antonucci 2004;Elitzur & Shlosman 2006;Perlman et al 2007;van der Wolk et al 2010). Accordingly, all low luminosity AGN should have been Type I sources, which of course is not the case.…”

Section: Discussionmentioning

confidence: 98%

The dichotomy of Seyfert 2 galaxies: intrinsic differences and evolution

Koulouridis

2014

A&A

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We present a study of the local environment (≤200 h −1 kpc) of 31 hidden broad line region (HBLR) and 43 non-HBLR Seyfert 2 (Sy2) galaxies in the nearby universe (z ≤ 0.04). To compare our findings, we constructed two control samples that match the redshift and the morphological type distribution of the HBLR and non-HBLR samples. We used the NASA Extragalactic Database (NED) to find all neighboring galaxies within a projected radius of 200 h −1 kpc around each galaxy, and a radial velocity difference δu ≤ 500 km s −1 . Using the digitized Schmidt survey plates (DSS) and/or the Sloan Digital Sky Survey (SDSS), when available, we confirmed that our sample of Seyfert companions is complete. We find that, within a projected radius of at least 150 h −1 kpc around each Seyfert, the fraction of non-HBLR Sy2 galaxies with a close companion is significantly higher than that of their control sample, at the 96% confidence level. Interestingly, the difference is due to the high frequency of mergers in the non-HBLR sample, seven versus only one in the control sample, while they also present a high number of hosts with signs of peculiar morphology. In sharp contrast, the HBLR sample is consistent with its control sample. Furthermore, the number of the HBLR host galaxies that present peculiar morphology, which probably implies some level of interactions or merging in the past, is the lowest in all four galaxy samples. Given that the HBLR Sy2 galaxies are essentially Seyfert 1 (Sy1) with their broad line region (BLR) hidden because of the obscuring torus, while the non-HBLR Sy2 galaxies probably also include true Sy2s that lack the BLR as well as heavily obscured objects that prevent even the indirect detection of the BLR, our results are discussed within the context of an evolutionary sequence of activity triggered by close galaxy interactions and merging. We argue that the non-HBLR Sy2 galaxies may represent different stages of this sequence, possibly the beginning and the end of the nuclear activity.

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“…Their estimate gives a smaller quantity of dust at a higher temperature. The possible presence of dust near the nucleus of M 87 was inferred from spectroscopic observations with Spitzer IRS, which showed an excess emission over the synchrotron component between 30 and 34 μm, the longest observed wavelengths (Perlman et al 2007). An alternative analysis of IRS spectra by Buson et al (2009) in the region up to 24 μm found no sign of dust emission: their MIR spectrum up to 24 μm can be completely explained by a combination of a stellar contribution and a synchrotron component.…”

Section: Dust Mass and Temperaturementioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Alighieri

Bianchi

Pappalardo

et al. 2013

A&A

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Aims. We study the dust content of a large optical input sample of 910 early-type galaxies (ETG) in the Virgo cluster, also extending to the dwarf ETG, and examine the results in relation to those on the other cold ISM components. Methods. We have searched for far-infrared emission in all galaxies in the input sample using the 250 μm image of the Herschel Virgo Cluster Survey (HeViCS). This image covers a large fraction of the cluster with an area of ∼55 square degrees. For the detected ETG we measured fluxes in five bands from 100 to 500 μm, and estimated the dust mass and temperature with modified black-body fits. Results. Dust is detected above the completeness limit of 25.4 mJy at 250 μm in 46 ETG, 43 of which are in the optically complete part of the input sample. In addition, dust is present at fainter levels in another six ETG. We detect dust in the four ETG with synchrotron emission, including M 87. Dust appears to be much more concentrated than stars and more luminous ETG have higher dust temperatures. Considering only the optically complete input sample and correcting for the contamination by background galaxies, dust detection rates down to the 25.4 mJy limit are 17% for ellipticals, about 40% for lenticulars (S0 + S0a), and around 3% for dwarf ETG. Dust mass does not correlate clearly with stellar mass and is often much greater than expected for a passive galaxy in a closedbox model. The dust-to-stars mass ratio anticorrelates with galaxy luminosity, and for some dwarf ETG reaches values as high as for dusty late-type galaxies. In the Virgo cluster slow rotators appear more likely to contain dust than fast ones. Comparing the dust results with those on Hi there are only eight ETG detected both in dust and in Hi in the HeViCS area; 39 have dust but only an upper limit on Hi, and eight have Hi but only an upper limit on dust. The locations of these galaxies in the cluster are different, with the dusty ETG concentrated in the densest regions, while the Hi rich ETG are at the periphery.

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The Mid‐Infrared Emission of M87

Cited by 60 publications

References 58 publications

Low-luminosity AGNs

Low-luminosity AGNs

The dichotomy of Seyfert 2 galaxies: intrinsic differences and evolution

TheHerschelVirgo Cluster Survey

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