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T1ο further evolujon of a galaxy depends critically o1 its orbit (sec. οσοι, Vollmer et al. | The further evolution of a galaxy depends critically on its orbit (see, e.g., Vollmer et al. |
2001). 1.0. a highly eccentric orbit wil lead the galaxy at a lieh velocity iuto t10 cluster οςxe. where the intracluster medium is deISCS and rau pressure will be very ποιο, | 2001), i.e. a highly eccentric orbit will lead the galaxy at a high velocity into the cluster core, where the intracluster medium is densest and ram pressure will be very strong. |
Recently. Voher (2009) esablished a model-based rai pressure strippi1οo time sequence of Virgo spiral galaxies. | Recently, Vollmer (2009) established a model-based ram pressure stripping time sequence of Virgo spiral galaxies. |
Snapshots of threc-dimeusioual models iucludius rani pressure Were compared to the observ«d easons distributions alc velocity fields. | Snapshots of three-dimensional models including ram pressure were compared to the observed gas distributions and velocity fields. |
The 3D velocity vector from the αναnica model and the timestep of the best-fit model has to be cousistent with the ealaxws projected position and radial velocity within the Vireo cluster. | The 3D velocity vector from the dynamical model and the timestep of the best-fit model has to be consistent with the galaxy's projected position and radial velocity within the Virgo cluster. |
Moreover. Vollmer (2009) concluded that the linear orbital segments derived. from the dynamical models together with the iutracluster iuediuu density distribution derived. fromm N-rav observations are consistent with the dynamical simulations of 6 Vireo cluster spirals. | Moreover, Vollmer (2009) concluded that the linear orbital segments derived from the dynamical models together with the intracluster medium density distribution derived from X-ray observations are consistent with the dynamical simulations of 6 Virgo cluster spirals. |
The deduced closest approach of the galaxies to the cluster ceuter (AL 87) is vetween 200 aud 600 pc. | The deduced closest approach of the galaxies to the cluster center (M 87) is between $200$ and $600$ kpc. |
Another consequence of ougoing rani presstre can be ound in the distribution of polarized radio coutinmnm cluission. | Another consequence of ongoing ram pressure can be found in the distribution of polarized radio continuum emission. |
Poluidzed radio ουπαπι eniüsson ds seusiive ο gas compression and shear motions. | Polarized radio continuum emission is sensitive to gas compression and shear motions. |
Asvuiuueric rkges of polarized radio contimmuni oenüssion are Tequeitly observed in Vireo spiral galaxies with disturbed Or runcated disks (Wezeeowiec ct al. | Asymmetric ridges of polarized radio continuum emission are frequently observed in Virgo spiral galaxies with disturbed or truncated disks (Weżggowiec et al. |
2007. Volmere al. | 2007, Vollmer et al. |
20073. | 2007). |
MIID modelling based ou the velocity fic‘ds of the οπασα model can corroborate a rai pressure strippiug scenario and/or discriminate between diftereut 1iteraclon SCOHALIOS (NGC σοι, Soida ct al. | MHD modelling based on the velocity fields of the dynamical model can corroborate a ram pressure stripping scenario and/or discriminate between different interaction scenarios (NGC 4654, Soida et al. |
2006: NGC 1522. Volhuer e al. | 2006; NGC 4522, Vollmer et al. |
2006: NCC 1501. Vollmer et al. | 2006; NGC 4501, Vollmer et al. |
2008). | 2008). |
Despite these clear sigus of ram pressure stripping ou the atomic gas content. only a handful of eas tails associate to cluster spiral galaxies lave been detected πι N-ravs: in ACO 2125 (C153 at z = 0.253. Wane ct al. | Despite these clear signs of ram pressure stripping on the atomic gas content, only a handful of gas tails associated to cluster spiral galaxies have been detected in X-rays: in ACO 2125 (C153 at z = 0.253, Wang et al. |
2001). in ACO 1367 (UCC 6697 at z = 0.022. Sun Vikhlinin 2005). in the Coma cluster (NGC 1515. Finoenenoy et al. | 2004), in ACO 1367 (UGC 6697 at z = 0.022, Sun Vikhlinin 2005), in the Coma cluster (NGC 4848, Finoguenov et al. |
2001). aid in ACO 3627 (ESO 137-001. Sun et al. | 2004), and in ACO 3627 (ESO 137-001, Sun et al. |
2006). | 2006). |
During a ram pressure stripping event it is expected that ooOeas is heated to N-vay teniperature by bow shocks. heat coucuction. and the mixine of the stripped ISAL iuto the hot iutracluster πουπια (ce... Stevens et al. | During a ram pressure stripping event it is expected that gas is heated to X-ray temperature by bow shocks, heat conduction, and the mixing of the stripped ISM into the hot intracluster medium (e.g., Stevens et al. |
1999. Schulz Sruck 2001. Roediger et al. | 1999, Schulz Struck 2001, Roediger et al. |
2006. Roedieer Briigeecu 2008. Tounesen Bivan 2009). | 2006, Roediger Brügggen 2008, Tonnesen Bryan 2009). |
So it is rather surISIE aud not clear why the N-rvay detection rate is so low. | So it is rather surprising and not clear why the X-ray detection rate is so low. |
IL paricular. there is no detection of the leading vow shock of a cluster spiral ealaxy iu the literature to our krowledge (Rasmussen et al. | In particular, there is no detection of the leading bow shock of a cluster spiral galaxy in the literature to our knowledge (Rasmussen et al. |
2006 detected a shock-like feaure 1i1 NGC 2276 which is part of the NCC 2300 eroup of ealaxies). | 2006 detected a shock-like feature in NGC 2276 which is part of the NGC 2300 group of galaxies). |
Since galaxies move with velocities between 1000 and 2000 + and the sound speed in the intracluster medium of the Vireo cluster is ~ 500-700 |. a bow shock with an associated Mach cone is expected. | Since galaxies move with velocities between $1000$ and $2000$ $^{-1}$ and the sound speed in the intracluster medium of the Virgo cluster is $\sim 500$ $700$ $^{-1}$, a bow shock with an associated Mach cone is expected. |
Tn this article we use NADINewton data to search for N-rav signatures of 3 radii xessure stripped spiral ealaxies belonging to the rai pressure stripping sequence | In this article we use XMM-Newton data to search for X-ray signatures of 3 ram pressure stripped spiral galaxies belonging to the ram pressure stripping sequence |
vear (data now sampled according to the timescale fit) are l32ruuuJv (1999.8). 172nuuJw. (2000.5). aud 215nuuJw (2001.3). | year (data now sampled according to the timescale fit) are mJy $.$ 8), mJy $.$ 5), and mJy $.$ 3). |
It is possible that the source became brighter at 5GGIIz iun outbursts at certain epochs: in particular around February 2001 (NEJD ~ 51900). | It is possible that the source became brighter at GHz in outbursts at certain epochs: in particular around February 2001 (MJD $\sim$ 51900). |
ILowever. because of the extrenuty of the variations aud the nuuber of sciutles. observed per run. we cannot distinguish this possibility from a steady brighltenimg. | However, because of the extremity of the variations and the number of scintles observed per run, we cannot distinguish this possibility from a steady brightening. |
We have no evidence for structure on arcsecond or arcnünute scales in this source. | We have no evidence for structure on arcsecond or arcminute scales in this source. |
From the radio spectra. (Paper D we do not expect any such structures to coutribute inore than a few αν. | From the radio spectrum (Paper I) we do not expect any such structures to contribute more than a few mJy. |
We have looked for evidence of extended structure by mapping several 12hhour ruus. | We have looked for evidence of extended structure by mapping several hour runs. |
We removed bv amplitude selt-calibratiue the whole uu ou the mean flux density. | We removed by amplitude self-calibrating the whole run on the mean flux density, |
When applied to AGNs belonging to very different classes, the multi-blob model deduces very similar properties for the size of the TeV emitting zones and the values of the magnetic field. | When applied to AGNs belonging to very different classes, the multi-blob model deduces very similar properties for the size of the TeV emitting zones and the values of the magnetic field. |
Furthermore the inferred bulk Lorentz factors I, can usually remain below value of 10, thus reconciling SSC models with (GR)MHD models,a except for the interpretation of the y-ray bump of AA in terms of synchrotron emission (see the green lines in Fig. [7)). | Furthermore the inferred bulk Lorentz factors $\Gamma_b$ can usually remain below a value of 10, thus reconciling SSC models with (GR)MHD models, except for the interpretation of the $\gamma$ -ray bump of A in terms of synchrotron emission (see the green lines in Fig. \ref{fig:CenA_SED}) ). |
A rather unified picture seems therefore to come out from the analysis. | A rather unified picture seems therefore to come out from the analysis. |
In our scenario, we locate the X- and y-ray emitting region in the jet formation zone, with opening angle larger than in the global VLBI radio zone, which is more distant from the core and mainly located in a region where the jet is more collimated. | In our scenario, we locate the X- and $\gamma$ -ray emitting region in the jet formation zone, with opening angle larger than in the global VLBI radio zone, which is more distant from the core and mainly located in a region where the jet is more collimated. |
This is somewhat reminiscent of a proposal made several years ago by ? for unifying X-ray and radio selected LLac objects. | This is somewhat reminiscent of a proposal made several years ago by \citet{1993ApJ...416..118C} for unifying X-ray and radio selected Lac objects. |
? showed that such a picture can be coherent with statistics of the LLac population. | \citet{1993ApJ...416..118C} showed that such a picture can be coherent with statistics of the Lac population. |
Since our model accounts for the observation with rather low bulk Lorentz factors and with large effective opening angles, we have found a way out of the problem of statistics on the number of detected TeV sources invoked by ?,, and we can reconcile beamed and unbeamed sources. | Since our model accounts for the observation with rather low bulk Lorentz factors and with large effective opening angles, we have found a way out of the problem of statistics on the number of detected TeV sources invoked by \citet{2006ApJ...640..185H}, and we can reconcile beamed and unbeamed sources. |
One important consequence of our proposal is that bright radio LLacs should be TeV emitters. | One important consequence of our proposal is that bright radio Lacs should be TeV emitters. |
This can be tested by further Observations. | This can be tested by further observations. |
Indeed, ? shows that the common historical unified LBL/HBL scheme (the so-called “blazar sequence") seems to be ruled out by the discovery of “outliers” low-power LBL and high-power HBL sources. | Indeed, \citet{2007Ap&SS.tmp..190P} shows that the common historical unified LBL/HBL scheme (the so-called “blazar sequence”) seems to be ruled out by the discovery of “outliers” low-power LBL and high-power HBL sources. |
Hence it does not seem impossible that objects that are very different at first sight, like radiogalaxies such as AA, could be (faint) VHE emitters. | Hence it does not seem impossible that objects that are very different at first sight, like radiogalaxies such as A, could be (faint) VHE emitters. |
Furthermore the fact that 887 has already been detected in the TeV range is encouraging for a future detection of such radiogalaxies. | Furthermore the fact that 87 has already been detected in the TeV range is encouraging for a future detection of such radiogalaxies. |
In the case of 2273, this object would rather be a misaligned LBL-like object. | In the case of 273, this object would rather be a misaligned LBL-like object. |
However one should stress that the fact that mainly HBL have been detected up to now at VHE is certainly only a selection effect. | However one should stress that the fact that mainly HBL have been detected up to now at VHE is certainly only a selection effect. |
Thus a TeV detection of 2273 would not be very surprising. | Thus a TeV detection of 273 would not be very surprising. |
The scenario we propose here has an additional interest in the sense that it allows to solve the long standing paradox of the apparent absence of high superluminal motion at the base of radio jets of TeV LLacs. | The scenario we propose here has an additional interest in the sense that it allows to solve the long standing paradox of the apparent absence of high superluminal motion at the base of radio jets of TeV Lacs. |
In our model, some X- and y- emitting plasma blobs are moving close to the line of sight, thus allowing for instance AA and 00521—36 to be potentially seen at VHE, while standing in misaligned extended jets. | In our model, some X- and $\gamma$ -ray emitting plasma blobs are moving close to the line of sight, thus allowing for instance A and $-$ 36 to be potentially seen at VHE, while standing in misaligned extended jets. |
This statement agrees well with the most recent studies by ?? who show that viewing angles, opening angles and Lorentz factors of (sub-)parsec scale jets evaluated by radio observations are usually underestimated, thus reconciling absent superluminal motions inferred from radio observations with high Lorentz factors required by different families of TeV emission models. | This statement agrees well with the most recent studies by \citet{2006MNRAS.369.1287G,2007MNRAS.377..446G} who show that viewing angles, opening angles and Lorentz factors of (sub-)parsec scale jets evaluated by radio observations are usually underestimated, thus reconciling absent superluminal motions inferred from radio observations with high Lorentz factors required by different families of TeV emission models. |
? also underlines the possibility to reconcile various contradictory observations by considering jets with opening angles of a few degrees. | \citet{2006astro.ph..3728W} also underlines the possibility to reconcile various contradictory observations by considering jets with opening angles of a few degrees. |
Early studies by ? on y-ray observations of AGNs with EGRET also indicate that strong beaming is not required to account for TeV blazars observations. | Early studies by \citet{1995ApJ...447..103D} on $\gamma$ -ray observations of AGNs with EGRET also indicate that strong beaming is not required to account for TeV blazars observations. |
Two different variability time scales appear within our mutli-blob scenario. | Two different variability time scales appear within our mutli-blob scenario. |
The short time scale is related to the characteristic size of individual blobs, as already discussed. | The short time scale is related to the characteristic size of individual blobs, as already discussed. |
A longer time scale occurs in the case of rotating jets with helicoidal magnetic field. | A longer time scale occurs in the case of rotating jets with helicoidal magnetic field. |
This induces a rotation of the cap, and the lag between "on-blob" and “inter-blob” emission corresponds to a long term y-ray variability. | This induces a rotation of the cap, and the lag between “on-blob” and “inter-blob” emission corresponds to a long term $\gamma$ -ray variability. |
From MHD models, we infer a characteristic rotation time of the magnetic field of the order of one year in the observer frame for 887. | From MHD models, we infer a characteristic rotation time of the magnetic field of the order of one year in the observer frame for 87. |
This modulation could explain the variation of the VHE emission observed between low and high states in 2004 and 2005. | This modulation could explain the variation of the VHE emission observed between low and high states in 2004 and 2005. |
This would imply some periodicity in the TeV emission of AGNs, but on timescales hitherto not explored. | This would imply some periodicity in the TeV emission of AGNs, but on timescales hitherto not explored. |
Via loss of orbital angular momentum, the short period systems that survive a CEP may be brought into Roche contact with the WD. | Via loss of orbital angular momentum, the short period systems that survive a CEP may be brought into Roche contact with the WD. |
Such systems may have been detected as cataclysmic variables (CV) but not recognized as post-planetary systems. | Such systems may have been detected as cataclysmic variables (CV) but not recognized as post-planetary systems. |
If the donor is a massive planet with a rocky core, it may be possible for the core to survive the CV phase. | If the donor is a massive planet with a rocky core, it may be possible for the core to survive the CV phase. |
This would result in a WD-+rocky core short period binary. | This would result in a WD+rocky core short period binary. |
By utilizing stellar evolution models from the ZAMS through the post-MS, we have followed the orbital dynamics of binary systems in which the companion is a 1 M; planet, 10 M; brown dwarf, or 100 M; low-mass MS star. | By utilizing stellar evolution models from the ZAMS through the post-MS, we have followed the orbital dynamics of binary systems in which the companion is a 1 $M_{\rm J}$ planet, 10 $M_{\rm J}$ brown dwarf, or 100 $M_{\rm J}$ low-mass MS star. |
Our evolutionary models incorporate a range of mass-loss rates and stellar masses. | Our evolutionary models incorporate a range of mass-loss rates and stellar masses. |
Dynamically, the orbital evolution is subject to mass-loss (which acts to increase the separation) and tidal torques (which act to decrease the separation). | Dynamically, the orbital evolution is subject to mass-loss (which acts to increase the separation) and tidal torques (which act to decrease the separation). |
We employ two commonly used tidal prescriptions to investigate the differences during the post-MS. | We employ two commonly used tidal prescriptions to investigate the differences during the post-MS. |
In particular, we find the following: | In particular, we find the following: |
halo sirouudius the galaxy. | halo surrounding the galaxy. |
We do not fiud evidence of asviuuetne depolarization in this radio source (the so called Laing - Couriugton effect. Laing 1988: Carrington et al. I988)). | We do not find evidence of asymmetric depolarization in this radio source (the so called Laing - Garrington effect, Laing \cite{laing}; Garrington et al. \cite{garrington}) ). |
Asstunine the existence of a halo. this fact could be explained if the source main axis were Iviug close to the plane of the sky. | Assuming the existence of a halo, this fact could be explained if the source main axis were lying close to the plane of the sky. |
This oricutation. cousisteut with the morphological &vuunetry of the radio source. would explain the very low flux deusitv of the core Gf unificatiou schemes of radio-loud active ealactic nuclei (e.g. Autonucci 1993)) are correct). and favors J1835|620 beie a giaut radio galaxy. | This orientation, consistent with the morphological symmetry of the radio source, would explain the very low flux density of the core (if unification schemes of radio-loud active galactic nuclei (e.g. Antonucci \cite{antonucci}) ) are correct), and favors J1835+620 being a giant radio galaxy. |
The reasons for restarting. or more properly. amplifvine the activity in the core of J1835|620 remain a mister. | The reasons for restarting, or more properly, amplifying the activity in the core of J1835+620 remain a mystery. |
It is already. known that galaxy interaction and mereiug can trieecr unclear activity (Stockton Mackeuty. 1983: Baheall ct al. 1997)). | It is already known that galaxy interaction and merging can trigger nuclear activity (Stockton Mackenty \cite{stockton}; ; Bahcall et al. \cite{bahcall}) ). |
Our optical image shows that the radio core of J1835|620 resides in a galaxy which belougs to a eroup of at least three galaxies showing mareiual sigus of αιπα. interaction. | Our optical image shows that the radio core of J1835+620 resides in a galaxy which belongs to a group of at least three galaxies showing marginal signs of mutual interaction. |
It is thus tempting to sugeest that iuteractions in this group of galaxies could. be associated with the differeut stages of radio activity in J1835|620. | It is thus tempting to suggest that interactions in this group of galaxies could be associated with the different stages of radio activity in J1835+620. |
Deeper optical images and spectroscopy of the other wo nmenibers of the eroup might shed Πο into this conjecture. | Deeper optical images and spectroscopy of the other two members of the group might shed light into this conjecture. |
Other interpretatious for J1835|620 could in principle ve considered. | Other interpretations for J1835+620 could in principle be considered. |
Clarke et al. (1992)) | Clarke et al. \cite{clarke2}) ) |
proposed. aud applied ou 3C219. a “passive inagnetie field” model iu which he observed jet iuteruptiouns would be a consequeuce of a transition from) a dominant axial magnetic field o a dominant toroidal feld occurring at the positio- where a force balance between a continuous jet and he surrounding iuediuni is attained. | proposed, and applied on 3C219, a “passive magnetic field” model in which the observed jet interruptions would be a consequence of a transition from a dominant axial magnetic field to a dominant toroidal field occurring at the position where a force balance between a continuous jet and the surrounding medium is attained. |
Iowever. we do iof observe the predicted maguetic field transitions in J1835|620 (sce Fig 1)). reudering this wodel implausible. | However, we do not observe the predicted magnetic field transitions in J1835+620 (see Fig \ref{mapas}) ), rendering this model implausible. |
On the other hand. argunentsOo based on recollimation shocks to explain components N2 aud $2 have difficulty in explaining the extraordinary svunuetry of this source. | On the other hand, arguments based on recollimation shocks to explain components N2 and S2 have difficulty in explaining the extraordinary symmetry of this source. |
Radio aud. optical observations of J1835|620 have been preseuted. | Radio and optical observations of J1835+620 have been presented. |
The observations were made in the iaune of the study of a new sample of large augular size radio sources selected from the NVSS. | The observations were made in the frame of the study of a new sample of large angular size radio sources selected from the NVSS. |
The R-baud optical image shows a galaxy coincident with the radio core position. | The R-band optical image shows a galaxy coincident with the radio core position. |
There are other two galaxies closely secu in projection. | There are other two galaxies closely seen in projection. |
The προςπι of the core host galaxy shows a very weak σολπα, but prominent narrow cussion lines from which we determine a redshift += 0.518. | The spectrum of the core host galaxy shows a very weak continuum, but prominent narrow emission lines from which we determine a redshift $z=0.518$ . |
Consequently. with an angular racio size of BOSS. J1835|620 is classified as a ciant radio ealaxy. | Consequently, with an angular radio size of $3\arcmin.88$, J1835+620 is classified as a giant radio galaxy. |
J1835|620 shows a very peculiar radio structure. with two svaunetrie bright components within a typical Fauaroft-Rilev type II structure. | J1835+620 shows a very peculiar radio structure, with two symmetric bright components within a typical Fanaroff-Riley type II structure. |
Given the extraordinary sviunietrv of the radio source (Sl to NI aru-ratio = 1: 82 oO N2 arurratio = 0.95). we interpret it using the model of restarting activity iu radio galaxies. | Given the extraordinary symmetry of the radio source (S1 to N1 arm-ratio = 1; S2 to N2 arm-ratio = 0.95), we interpret it using the model of restarting activity in radio galaxies. |
Two distinct pliases of core activity would be responsible for the observed norpholoey. | Two distinct phases of core activity would be responsible for the observed morphology. |
Observational properties have been compared with xedietious from 2-D unmerical simulations by Clarke Durus 1991)). | Observational properties have been compared with predictions from 2-D numerical simulations by Clarke Burns \cite{clarke1}) ). |
The existence of a hot-spot in Nl ogether with spectral aging argunenuts indicate that NI and $1 are still supplied by. fresh particles. nuplving he existence of απ underlying jet counectiung the core with the outer compoucuts aud that the activity in J1835620 did not stop completely. | The existence of a hot-spot in N1 together with spectral aging arguments indicate that N1 and S1 are still supplied by fresh particles, implying the existence of an underlying jet connecting the core with the outer components and that the activity in J1835+620 did not stop completely. |
In consequence. the jew components N2 and $2 would represeut re result of a jew ejection propagating through the primary uudoerblviug jet. | In consequence, the new components N2 and S2 would represent the result of a new ejection propagating through the primary underlying jet. |
The parallel magnetic fields of components N2 aud S2 are consistent with a "secoud-phnase jet which is overdeuse with respect to the "fixst-phase one. | The parallel magnetic fields of components N2 and S2 are consistent with a “second-phase” jet which is overdense with respect to the “first-phase” one. |
Faraday votation of the polarization vectors is observed. with a RAL distributed rather wuiformly all over he source. | Faraday rotation of the polarization vectors is observed, with a $RM$ distributed rather uniformly all over the source. |
We sugeest that the rotation is produced by an ionized halo surrounding the radio source. | We suggest that the rotation is produced by an ionized halo surrounding the radio source. |
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