Electronically Available Publications and Pre-Prints of the Brandeis Radio Astronomy Group:

Jets from Sub-Parsec to Kiloparsec Scales: A Physical Connection, by F. Tavecchio, L. Maraschi (Brera), R.M. Sambruna (GMU), C.M. Urry (Yale), C.C. Cheung (Brandeis), J.K. Gambill (GMU), R. Scarpa (ESO). 2004, ApJ, accepted

ABSTRACT: The Chandra discovery of bright X-ray emission from kpc-scale jets allows insight into the physical parameters of the jet flow at large scale. At the opposite extreme, extensive studies of the inner relativistic jets in Blazars with multiwavelength observations, yield comparable information on sub-parsec scales. In the framework of simple radiation models for the emission regions we compare the physical parameters of jets on these two very different scales in the only two well studied Blazars for which large-scale emission has been resolved by Chandra. Notably, we find that the relativistic Doppler factors and powers derived independently at the two scales are consistent, suggesting that the jet does not suffer severe deceleration or dissipation. Moreover the internal equipartition pressures in the inner jet and in the external X-ray bright knots scale inversely with the jet cross section as expected in the simple picture of a freely expanding jet in equipartition.

High Levels of Circularly Polarized Emission from the Radio Jet in NGC 1275 (3C84), by D.C. Homan (NRAO, Denison) and J.F.C. Wardle (Brandeis). 2004, ApJL, accepted

ABSTRACT: We present multi-frequency, high resolution VLBA circular polarization images of the radio source 3C 84 in the center of NGC 1275. Our images reveal a complex distribution of circular polarization in the inner parsec of the radio jet, with local levels exceeding 3% polarization, the highest yet detected with VLBI techniques. The circular polarization changes sign along the jet, making 3C 84 also the first radio jet to show both signs of circular polarization simultaneously. The spectrum and changing sign of the circular polarization indicate that it is unlikely to be purely intrinsic to the emitted synchrotron radiation. The Faraday conversion process makes a significant and perhaps dominant contribution to the circular polarization, and the observed spectrum suggests the conversion process is near saturation. The sign change in the circular polarization along the jet may result from this saturation or may be due to a change in magnetic field order after an apparent bend in the jet. From the small spatial scales probed here, ~ 0.15 pc, and the comparably high levels of circular polarization inferred for the intra-day variable source PKS 1519-273, we suggest a connection between small spatial scales and efficient production of circular polarization.

A Survey of Extended Radio Jets with Chandra and HST, by R.M. Sambruna, J.K. Gambill (George Mason Univ.), L. Maraschi, F. Tavecchio, R. Cerutti (Oss Brera), C. C. Cheung (Brandeis Univ.), C. M. Urry (Yale Univ.), G. Chartas (Penn State Univ.), 2004, ApJ, accepted

ABSTRACT: We present the results from an X-ray and optical survey of a sample of 17 radio jets in AGN performed with Chandra and HST. The sample was selected from the radio and is unbiased toward detection at shorter wavelengths, but preferentially it includes beamed sources. We find that X-ray emission is common on kpc-scales, with over half radio jets exhibiting at least one X-ray knot on the Chandra images. The distributions of the radio-to-X-ray and radio-to-optical spectral indices for the detected jets are similar to the limits for the non-detections,suggesting all bright radio jets have X-ray counterparts which will be visible in longer observations. Comparing the radio and X-ray morphologies shows that the majority of the X-ray jets have structures that closely map the radio. Analysis of the SED of the jet knots suggest the knots in which the X-ray and radio morphologies track each other produce X-rays by IC scattering of the Cosmic Microwave Background. The remaining knots produce X-rays by the synchrotron process. Spectral changes are detected along the jets, with the ratio of the X-ray-to-radio and optical-to-radio flux densities decreasing from the inner to the outer regions. This suggests the presence of an additional contribution to the X-ray flux in the jet's inner part, either from synchrotron or IC of the stellar light. Alternatively, in a pure IC/CMB scenario, the plasma decelerates as it flows from the inner to the outer regions. Finally, the X-ray spectral indices for the brightest knots are flat, indicating that the bulk of the luminosity of the jets is emitted at GeV energies, and raising the interesting possibility of future detections with GLAST.

Parsec-Scale Blazar Monitoring: The Data , by Roopesh Ojha, Daniel C. Homan, David H. Roberts, John F. C. Wardle, Margo F. Aller, Hugh D. Aller, and Philip A. Hughes. 2004, ApJS, 150, 187:237

ABSTRACT: We present the images and modeling data obtained from a dual frequency, six-epoch, VLBA polarization experiment monitoring a sample of 12 blazars. The observations were made at 15 and 22 GHz at evenly spaced, bimonthly intervals over 1996. The advent of the VLBA makes possible a data set with reliable calibration as well as regular and frequent temporal sampling. Detection of circular polarization, proper motion studies, and flux and polarization variability in the sample are some of the topics that such a data set makes available for robust investigation.

Radio Identification of the X-ray Jet in the z=4.3 Quasar GB 1508+5714 , by C.C. Cheung (Brandeis). 2003, ApJL, accepted

ABSTRACT: The recent discovery of an X-ray jet in the z=4.3 quasar GB~1508+5714 by Yuan et al. (astro-ph/0309318) and Siemiginowska et al. (astro-ph/0310241) prompted a search for its radio counterpart. Here, we report the successful discovery of faint radio emission from the jet at 1.4 GHz using archival VLA data. The X-ray emission is best interpreted as inverse Compton (IC) emission off the CMB as discussed by the previous investigators. In this scenario, its high X-ray to radio monochromatic luminosity ratio, compared to previously detected IC/CMB X-ray jets at lower redshift, is a natural consequence of its high redshift.

The XMM-Newton View of the X-ray Halo and Jet of NGC 6251 , by R.M. Sambruna (1), M. Gliozzi (1), D. Donato (1), F. Tavecchio (2), C.C. Cheung (3), R. Mushotzky (4) ((1) GMU, (2) OAB Merate, (3) Brandeis University, (4) NASA GSFC). 2003, Astronomy and Astrophysics, accepted

ABSTRACT: We present an XMM observation of the radio jet and diffuse halo of the nearby radio galaxy NGC6251. The EPIC spectrum of the galaxy's halo is best-fitted by a thermal model with temperature kT~1.6 keV and subsolar abundances. Interestingly, an additional hard X-ray component is required to fit the EPIC spectra of the halo above 3 keV, and is independently confirmed by an archival Chandra observation. However, its physical origin is not clear. Contribution from a population of undetected Low Mass X-ray Binaries seems unlikely. Instead, the hard X-ray component could be due to inverse Compton scattering of the CMB photons off relativistic electrons scattered throughout the halo of the galaxy, or non-thermal bremsstrahlung emission. The IC/CMB interpretation, together with limits on the diffuse radio emission, implies a very weak magnetic field, while a non-thermal bremsstrahlung origin implies the presence of a large number of very energetic electrons. We also detect X-ray emission from the outer (~3.5') jet, confirming previous ROSAT findings. Both the EPIC and ACIS spectra of the jet are best-fitted by a power law with photon index \~1.2. A thermal model is formally ruled out by the data. Assuming an origin of the X-rays from the jet via IC/CMB, as suggested by energetic arguments, and assuming equipartition implies a large Doppler factor (delta~10). Alternatively, weaker beaming is possible for magnetic fields several orders of magnitude lower than the equipartition field.

Near-Infrared Observations of BL Lacertae Host Galaxies , by C. C. Cheung (1,4), C. Megan Urry (2,4), Riccardo Scarpa (3,4), and Mauro Giavalisco (4) (1) Brandeis Univ. (2) Yale Univ. (3) European Southern Observatory (4) STScI. 2003, ApJ, accepted

ABSTRACT: Multi-band near-infrared images of twelve BL Lacertae objects were obtained with the 2.5m telescope at the Las Campanas Observatory in order to determine the properties of their underlying host galaxies. Resolved emission was clearly detected in eight of the lowest redshift targets (up to z~0.3), and was modeled with a de Vaucouleurs r^{1/4} surface brightness law. We find that the morphologies match the elliptical galaxy profiles well, and that the BL Lac objects reside in large and luminous, but otherwise normal hosts -- consistent with previous studies done predominantly at optical wavelengths. The median absolute K-band magnitude of the galaxies in this study is -26.2, the average half-light radius is 4.2 +/- 2.3 kpc, and their average integrated R-K color is 2.7 +/- 0.3 mag. These are well within the range of values measured previously in the H-band by Kotilainen et al. and Scarpa et al. in a comparable number of targets. Taking their data together with our results, we find a best-fit K-band Kormendy relation of \mu_{e} = 4.3 log_{10} (r_{e}/kpc) + 14.2 mag arcsec^{-2}, virtually identical to that obtained for normal ellipticals. Finally, the near-infrared colors determined for five galaxies (average J-K = 0.8 +/- 0.3 mag) are the first such measurements for BL Lac hosts, and match those expected from old stellar populations at the BL Lac redshifts.

Theoretical Models for Producing Circularly Polarized Radiation in Extragalactic Radio Sources , by John F. C. Wardle (1) and Daniel C. Homan (2), (1) Brandeis Univ. (2) National Radio Astronomy Obs. 2003, To appear in the proceedings of "Circular Polarization of Relativistic Jet Sources", eds R. P. Fender and J.-P. Macquart, in Astrophysics and Space Science.

ABSTRACT: We discuss the production of circular polarization in compact radio sources both by the intrinsic mechanism and by Faraday conversion. We pay particular attention to the magnetic field structure, considering partially ordered fields and Laing sheets, and distinguishing between uniform and unidirectional fields. (The latter can be constrained by flux conservation arguments.) In most cases, Faraday conversion is the more important mechanism. Conversion opera tes on Stokes U, which can be generated by internal Faraday rotation, or by magnetic field fluctuations, which can therefore produce circular polarization even in a pure pair plasma. We also show that the spectrum of circular polarization in an inhomogeneous jet can be quite different from that in a uniform source, being flat or even inverted.

Chandra Observations of Nuclear X-ray Emission from a Sample of Radio Sources , by J. K. Gambill (1), R. M. Sambruna (1), G. Chartas (2), C. C. Cheung (3), L. Maraschi (4), F. Tavecchio (4), C. M. Urry (5), J. E. Pesce (1); (1) George Mason University, (2) Penn State University, (3) Brandeis University, (4) Osservatorio Astronomico di Brera, (5) Yale University; accepted for publication in Astronomy and Astrophysics

ABSTRACT: We present the X-ray properties of a sample of 17 radio sources observed with the Chandra X-ray Observatory as part of a project aimed at studying the X-ray emission from their radio jets. In this paper, we concentrate on the X-ray properties of the unresolved cores. The sample includes 16 quasars (11 core-dominated and 5 lobe-dominated) in the redshift range z=0.30--1.96, and one low-power radio-galaxy at z=0.064. No diffuse X-ray emission is present around the cores of the quasars, except for the nearby low-power galaxy that has diffuse emission on a scale and with a luminosity consistent with other FRIs. No high-amplitude, short-term variability is detected within the relatively short Chandra exposures. However, 1510-089 shows low-amplitude flux changes with a timescale of $\sim$25 minutes. The X-ray spectra of the quasar cores are generally well described by a single power law model with Galactic absorption. However, in six quasars we find soft X-ray excess emission below 1.6 keV. Interestingly, we detect an Fe K-shell emission line, consistent with fluorescent Kalpha emission from cold Iron, in one lobe- and two core-dominated sources. The average X-ray photon index for the quasars in the sample is Gamma=1.66 and dispersion, sigma=0.23. The average spectral slope for our sample is flatter than the slope found for radio-quiet quasars and for radio-loud AGNs with larger jet orientations; this indicates that beaming affects the X-ray emission from the cores in our sample of quasars.

New Detections of Optical Emission from Kiloparsec-scale Quasar Jets , by C. C. Cheung, J. F. C. Wardle, Tingdong Chen, and S. P. Hariton (Brandeis University). to appear in proceedings of: ``The Physics of Relativistic Jets in the Chandra and XMM Era,'' eds. G. Brunetti, D.E. Harris, R.M. Sambruna, and G. Setti, submitted to New Astronomy Review.

ABSTRACT: We report initial results from the detection of optical emission in the arcsecond-scale radio jets of two quasars utilizing images from the Hubble Space Telescope archive. The optical emission has a very knotty appearance and is consistent with synchrotron emission from highly relativistic electrons in the jet. Combining these observations with those of previously reported features in other quasars, an emerging trend appears to be that their radio-to-optical spectral indices are steeper than those of similar features in jets of lower power radio sources.

Chandra Observations of Three SDSS Quasars at z~6 , by D. A. Schwartz (Harvard-Smithsonian Center for Astrophysics), C. C. Cheung, J. F. C. Wardle (Brandeis University). to appear in proceedings of: ``Active Galactic Nuclei: from Central Engine to Host Galaxy,'' Meudon, July 2002 meeting; ASP Conference Series, Eds.: S. Collin, F. Combes and I. Shlosman

ABSTRACT: Chandra snapshot observations of the three most distant quasars then known, at redshifts 5.82, 5.99, and 6.28, gave signficant detections even in the short, 6 -- 8 ks, observations. The X-ray to optical luminosity ratios indicate that quasars will be detectable in X-rays if they exist at even larger redshifts. The present observations hint at two exciting discoveries. An extended X-ray source 23 arcsec from SDSS1306+0356 may be a jet emitting inverse Compton radiation from the Cosmic Microwave Background. SDSS 1030+0524 does not appear to be a point source, and may be a gravitationally lensed system, or contain a small scale X-ray jet.

Probing the Circular Polarization of Relativistic Jets on VLBI Scales , by Daniel C. Homan (1) and John F. C. Wardle (2) ((1) National Radio Astronomy Obs. (2) Brandeis Univ.), 2002. To appear in the proceedings of "Circular Polarization of Relativistic Jet Sources", eds R. P. Fender and J.-P. Macquart, in Astrophysics and Space Science.

ABSTRACT: High resolution studies of circular polarization allow us see where it arises in a jet, study its local fractional level and spectrum, and compare these results to local measures of linear polarization and Faraday rotation. Here we not only review past results from Very Long Baseline Array (VLBA) circular polarization studies, but we also present preliminary new results on two quasars. In the core of PKS 0607-157, we find strong circular polarization at 8 GHz and much weaker levels at 15 GHz. Combined with the linear polarization data, we favor a simple model where the circular is produced by Faraday conversion driven by a small amount of Faraday rotation. In the core of 3C345, we find strong circular polarization at 15 GHz in a component with distinct linear polarization. This core component is optically thick at 8 GHz, where we detect no circular polarization. With opposite trends in frequency for PKS 0607-157 and 3C345, it seems clear that local conditions in a jet can have a strong effect on circular polarization and need to be taken into account when studying inhomogeneous objects with multi-frequency observations.

Detection of Optical Synchrotron Emission from the Radio Jet of 3C279 , by C. C. Cheung, Brandeis University, 2002. Accepted for publication in The Astrophysical Journal Letters.

ABSTRACT: We report the detection of optical and ultraviolet emission from the kiloparsec scale jet of the well-known quasar 3C~279. A bright knot, discovered in archival V and U band Hubble Space Telescope Faint Object Camera images, is coincident with a peak in the radio jet ~0.6 arcsec from the nucleus. The detection was also confirmed in Wide Field Planetary Camera-2 images. Archival Very Large Array and MERLIN radio data are also analyzed which help to show that the high-energy optical/UV continuum, and spectrum, are consistent with a synchrotron origin from the same population of relativistic electrons responsible for the radio emission.

PKS 1510-089: A Head-On View of a Relativistic Jet , by Daniel C. Homan (1), John F.C. Wardle (2), Chi C. Cheung (2), David H. Roberts (2), Joanne M. Attridge (3) ((1) NRAO, (2) Brandeis University, (3) MIT Haystack Observatory), 2002. Accepted for publication in The Astrophysical Journal.

ABSTRACT: The gamma-ray blazar PKS 1510-089 has a highly superluminal milli-arcsecond jet at a position angle (PA) of -28 degrees and an arcsecond jet with an initial PA of 155 degrees. With a PA difference of 177 degrees between the arcsecond and milli-arcsecond jets, PKS 1510-089 is perhaps the most highly misaligned radio jet ever observed and serves as a graphic example of projection effects in a highly beamed relativistic jet. Here we present the results of observations designed to bridge the gap between the milli-arcsecond and arcsecond scales. We find that a previously detected ``counter-feature'' to the arcsecond jet is directly fed by the milli-arcsecond jet. This feature is located 0.3'' from the core, corresponding to a de-projected distance of 30 kiloparsecs. The feature appears to be dominated by shocked emission and has an almost perfectly ordered magnetic field along its outside edge. We conclude that it is most likely a shocked bend, viewed end-on, where the jet crosses our line of sight to form the southern arcsecond jet. While the bend appears to be nearly 180 degrees when viewed in projection, we estimate the intrinsic bending angle to be between 12 and 24 degrees. The cause of the bend is uncertain; however, we favor a scenario where the jet is bent after it departs the galaxy, either by ram pressure due to winds in the intracluster medium or simply by the density gradient in the transition to the intergalactic medium.

A Survey of Extended Radio Jets in AGN with Chandra and HST: First Results , by Rita M. Sambruna (George Mason Univ.), L. Maraschi, F. Tavecchio (Oss Brera), C. Megan Urry (Yale Univ.), C. C. Cheung (Brandeis Univ.), G. Chartas (Penn State Univ.), R. Scarpa (ESO), Jessica K. Gambill (George Mason Univ.) 2002. Accepted for publication in The Astrophysical Journal.

ABSTRACT: We present the first results from an X-ray and optical survey of a sample of AGN radio jets with Chandra and HST. We focus here on the first six sources observed at X-rays, in four of which a bright X-ray jet was detected for the first time. In three out of four cases optical emission from the jet is also detected in our HST images. We compare the X-ray morphology with the radio as derived from improved processing of archival VLA data and we construct spectral energy distributions (SED) for the most conspicuous emission knots. In most cases the SEDs, together with the similarity of the X-ray and radio morphologies, favor an inverse Compton origin of the X-rays. The most likely origin of the seed photons is the Cosmic Microwave Background, implying the jets are still relativistic on kiloparsec scales. However, in the first knot of the PKS 1136-135 jet, X-rays are likely produced via the synchrotron process. In all four cases bulk Lorentz factors of a few are required. The radio maps of the two jets not detected by either Chandra or HST suggest that they are less beamed at large scales than the other four detected sources. Our results demonstrate that, at the sensitivity and resolution of Chandra, X-ray emission from extragalactic jets is common, yielding essential information on their physical properties.

Parsec-Scale Blazar Monitoring: Flux and Polarization Variability, by Daniel C. Homan, Roopesh Ojha, John F. C. Wardle, David H. Roberts, Margo F. Aller, Hugh D. Aller, Philip A. Hughes. 2001. Submitted to The Astrophysical Journal.

ABSTRACT: We present analysis of the flux and polarization variability of parsec scale radio jets from a dual-frequency, six-epoch, VLBA polarization experiment monitoring 12 blazars. The observations were made at 15 and 22 GHz at bimonthly intervals over 1996. Here we analyze the flux, fractional polarization, and polarization position angle behavior of core regions and jet features, considering both the linear trends of these quantities with time and more rapid fluctuations about the linear trends. The dual frequency nature of the observations allows us to examine spectral evolution, to separate Faraday effects from changes in magnetic field order, and also to deduce empirical estimates for the uncertainties in measuring properties of VLBI jet features (see the Appendix). [abridged]

Detection of an X-ray jet in 3C 371 with Chandra, by Joseph E. Pesce, Rita M. Sambruna, F. Tavecchio, L. Maraschi, C. C. Cheung, C. Megan Urry, and R. Scarpa. 2001. Accepted by The Astrophysical Journal Letters. Figure 1 (in color) is available in GIF format or as a high resolution Postscript.

ABSTRACT: We report the detection at X-rays of the radio/optical jet of 3C 371, from a short (10 ks) Chandra exposure in March 2000. We also present a new MERLIN observation at 1.4 GHz together with a renalysis of the archival HST WFPC2 F555W image. Despite the limited signal-to-noise ratio of the Chandra data, the X-ray morphology is clearly different from that of the radio/optical emission, with the brightest X-ray knot at 1.7" from the nucleus and little X-ray emission from the brightest radio/optical knot at 3.1". We construct the spectral energy distributions for the two emission regions at 1.7" and 3.1". Both show that the X-ray flux is below the extrapolation from the radio-to-optical continuum, suggesting moderately beamed synchrotron from an electron population with decreasing high energy cut-off as a plausible emission mechanism.

Making Movies from Radio Astronomical Images with AIPS, by C. C. Cheung, D. C. Homan, J. F. C. Wardle, D. H. Roberts. 2001. NRAO AIPS Memo # 106.

ABSTRACT: We present a detailed recipe for making movies from multi-epoch radio observations of astronomical sources. Images are interpolated linearly in time to create a smooth succession of frames so that a continuous movie can be compiled. Here, we outline the procedure, and draw attention to specific details necessary for making a successful movie. In particular, we discuss the issues pertaining specifically to making polarization movies. The procedure described here has been implemented into scripts in NRAO's AIPS package (Brandeis AIPS Movie Maker -- BAMM) that are available for public use (http://www.astro.brandeis.edu).

Parsec-Scale Circular Polarization Observations of 40 Blazars, by D. C. Homan, J. M. Attridge, and J. F. C. Wardle. 2001. Accepted by The Astrophysical Journal.

ABSTRACT: We present circular polarization results from a 5 GHz survey of the parsec-scale polarization properties of 40 AGN made with the VLBA. We find 11 circular polarization detections at the 3 sigma level or higher. This nearly quadruples the number of sources detected in circular polarization at VLBI resolution. We find no correlation between fractional linear and circular polarization across our sample. A likely explanation is external Faraday depolarization in the cores of AGN which reduces linear polarization but leaves circular polarization unchanged. In comparing ours and other recent results to observations made ~ 20 years ago, we find that, in five of six cases, sources have the same sign of circular polarization today as they did 20 years ago. This suggests the presence of a long term property of the jets, such as the polarity of a net magnetic flux, which is stable on time-scales much longer than those of individual outbursts.

Parsec-Scale Blazar Monitoring: Proper Motions, by D. C. Homan, R. Ojha, J. F. C. Wardle, D. H. Roberts, M. F. Aller, H. D. Aller, and P. A. Hughes. Appeared in The Astrophysical Journal 2001, vol 549, p. 840.

ABSTRACT: We present proper motions obtained from a dual frequency, six-epoch, VLBA polarization experiment monitoring a sample of 12 blazars. The observations were made at 15 GHz and 22 GHz at bi-monthly intervals over 1996. Ten of the eleven sources for which proper motion could be reliably determined are superluminal. Only J2005+77 has no superluminal components. Three sources (OJ287, J1224+21, and J1512-09) show motion faster than 10h^{-1} c, requiring $\gamma_{pattern}$ of at least 10h^{-1} (H_0 = 100h km/s/Mpc). We compare our results to those in the literature and find motions outside the previously observed range for four sources. While some jet components exhibit significant non-radial motion, most motion is radial. In at least two sources there are components moving radially at significantly different structural position angles. In five of six sources (3C120, J1224+21, 3C273, 3C279, J1512-09, and J1927+73) that have multiple components with measurable proper motion, the innermost component is significantly slower than the others, suggesting that acceleration occurs in the jet. In the motions of individual components we observe at least one decelerating motion and two ``bending'' accelerations which tend to align their motions with larger scale structure. We also discuss in detail our procedures for obtaining robust kinematical results from multi-frequency VLBI data spanning several epochs.

The Nature of Jets: Evidence from Circular Polarization Observations, by John F. C. Wardle, Daniel C. Homan. To appear in "Particles and Fields in Radio Galaxies", Eds. Robert A. Laing and Katherine M. Blundell, ASP Conference Series

ABSTRACT: We review recent observations of circularly polarized radiation from AGN made with the VLBA and with the ATCA. We also discuss briefly the detections of the Galactic sources Sag A* and SS433. The origin of the circular polarization is still an open question in most cases, and we discuss four possible mechanisms. Detectable circular polarization is a common property of quasars, but not of radio galaxies, and is always associated with the compact core. There is growing evidence that the sign of the circular polarization stays the same over at least two or three decades in time, suggesting it is a fundamental property of the jet.

Direct Distance Measurements to Superluminal Radio Sources, by D. C. Homan and J. F. C. Wardle. Appeared in The Astrophysical Journal (2000) vol 535, pg. 575.

ABSTRACT: We present a new technique for directly measuring the distances to superluminal radio sources. By comparing the observed proper motions of components in a parsec scale radio jet to their measured Doppler factors, we can deduce the distance to the radio source independent of the standard rungs in the cosmological distance ladder. This technique requires that the jet angle to the line of sight and the ratio of pattern to flow velocities are sufficiently constrained. We evaluate a number of possibilities for constraining these parameters and demonstrate the technique on a well defined component in the parsec scale jet of the quasar 3C279 (z = 0.536). We find an angular size distance to 3C279 of greater than 1.8 (+0.5,-0.3) n^{1/8} Gpc, where n is the ratio of the energy density in the magnetic field to the energy density in the radiating particles in that jet component. For an Einstein-de Sitter Universe, this measurement would constrain the Hubble constant to be H < 65 n^{-1/8} km/s/Mpc at the two sigma level. Similar measurements on higher redshift sources may help discriminate between cosmological models.

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1999 and before

Detection and Measurement of Parsec-Scale Circular Polarization in Four AGN, by D. C. Homan and J. F. C. Wardle. Appeared in The Astronomical Journal (1999) vol 118, pg 1942. [also in PDF format]


ABSTRACT: We present five epochs of 15 GHz VLBA observations of 13 AGN. These observations were specially calibrated to detect parsec scale circular polarization and our calibration techniques are discussed and analyzed in detail. We obtained reliable detections of parsec scale circular polarization in the radio jets of 4 AGN: 3C84, PKS 0528+134, 3C273, and 3C279. For each of these objects our detections are at the level of ~ 0.3-1% local fractional circular polarization. Our observations are consistent across multiple epochs (and different calibration techniques) in the sign and magnitude of the circular polarization observed. 3C273 and 3C279 both undergo core outbursts during our observations and changes in the circular polarization of both sources are correlated with these outbursts. In general, we observe the circular polarization to be nearly coincident with the strong VLBI cores of these objects; however, in 3C84 the circular polarization is located a full milli-arcsecond south of the source peak, and in the 1996.73 epoch of 3C273 the circular polarization is predominately associated with the newly emerging jet component. Our observations support the theoretical conclusion that emission of circular polarization is a sensitive function of opacity, being strongest when the optical depth is near unity. Circular polarization may be produced as an intrinsic component of synchrotron radiation or by the Faraday conversion of linear to circular polarization. Our single frequency observations do not easily distinguish between these possible mechanisms, but independent of mechanism, the remarkable consistency across epoch of the sign of the observed circular polarization suggests the existence of a long term, stable, uni-directional magnetic field. Single dish observations of 3C273 and 3C279 at 8 GHz by Hodge and Aller suggest that this stability may persist for decades in our frame of observation.

Radio Jet-Ambient Medium Interactions on Parsec Scales in the Blazar 1055+018, by J. M. Attridge, D. H. Roberts, and J. F. C. Wardle. Appeared in Astrophys.J. (1999) vol 518, pg. 87.


ABSTRACT: As part of our study of the magnetic fields of AGN we have recently observed a large sample of blazars with the Very Long Baseline Array. Here we report the discovery of a striking two-component jet in the source 1055+018, consisting of an inner spine with a transverse magnetic field, and a fragmentary but distinct boundary layer with a longitudinal magnetic field. The polarization distribution in the spine strongly supports shocked-jet models while that in the boundary layer suggests interaction with the surrounding medium. This behavior suggests a new way to understand the differing polarization properties of strong- and weak-lined blazars.

Electron-positron Jets Associated with the Quasar 3C279, by J. F. C. Wardle, D. C. Homan, R. Ojha, and D. H. Roberts. Appeared in Nature (1998) vol 395, pg. 457. [also in PDF format]


ABSTRACT: A long outstanding problem in extragalactic astrophysics is the composition of the relativistic jets of plasma streaming from the nuclei of quasars and active galaxies -- whether it is predominantly a "normal" (electron - proton) plasma, or a "pair" (electron - positron) plasma. Distinguishing between these possibilities is crucial for understanding the physical processes occuring close to the putative supermassive black holes in galactic nuclei that create the jets. Here we present a new approach to the problem of jet composition, by detecting circularly polarized radio emission from the archtypal quasar 3C279, using the VLBA. The circular polarization is produced by Faraday conversion, which requires that the energy distribution of the radiating particles extends to very low energies, indicating that electron - positron pairs are a major component of the jet plasma. Similar detections in three other radio sources, suggest that in general, extragalactic radio jets are composed primarily of an electron - positron plasma.