Notes on Tanami Sources

• 0047-579

  • QSO with z=1.797 (Peterson et al. 1976)
  • map: two components, core + component WNW, separation 20mas (Ojha et al. 2005)
  • map: core extended symetrically (WNW,ESE) (Preston et al. 1989)

• 0208-512

  • map: compact core extended to SW (Ojha et al. 2004)
  • map: compact core + additional component (slight extension to SW) superluminal candidate, from model fit parameters (1992,1993) proper motion of 0.6mas/yr, corresponding to a transverse velocity of 16,8c (H_0=100, q_0=0.5), from ROSAT measurement of 0.22 microJansky at 1keV (Dondi & Ghisellini 1995): lower limit of Doppler factor 10.2 (Shen et al. 1998)
  • X-ray emission of core and 4'' jet to SW revealed by Chandra (Marshall et al. 2005)
  • HPQ (highly polarized quasar) (Impey & Tapia 1988, 1990)
  • second southern AGN detected at gamma-ray energies (Bertsch at al. 1993, Blom et al. 1995)
  • one of the hardest spectra (von Montigny et al. 1995, Chiang et al. 1995)
  • Gamma-ray Blazar (Tavecchio et al. 2007)

• 0332-403

  • map: compact core (no clear additional components in the mas scale) (Ojha et al. 2004)
  • map: compact core slightly extended to the east, redshift may be wrong (This value is from the Catalogue of Quasi Stellar-Objects (Barbieri, Capaccioli, & Zambon 1975), in which the reference was incorrect.) (Shen et al. 1998)
  • different map, small jet component to the west, separation ~2mas (Fomalont et al. 2000)
  • HPQ (p = 14% ?), z=1.445 is doubted strongly in several papers (Tornikoski et al. 2001)

• 0405-385

  • one of 3 unusually strong IDV sources (other two: PKS 1257-326 and J1819+385) extreme example of intra-day variability (IDV) one of three IDV sources, possibly caused by interstellar scintillation (ISS) (Kedziora-Cudczer et al. 2006,..., 1997, 1996)
  • component to the west at 1.5 mas, compatible with the RRFID images (Zensus et al. 2002)
  • 2003 November: component to the west at 4 mas (Ojha et al. 2005)
  • rapid variability in the flux density on hourly time scales, alternation between long periods (years) of quiescence and short (a few months) periods of intense activity (Cimo et al. 2004)

• 0438-436

  • radio-loud, core-dominated, highly polarized quasar (Impey & Tapia 1988)
  • first X-ray spectrum of a high-redshift quasar (z=2.85), strong soft X-ray absorption (probably intrinsic) (Wilkes et al. 1992)
  • from Brocksopp et al. 2004: radio-loud, high-redshift source z=2.852, spectrum with redshifted absorption
  • two components aligned in SE (separation 35mas), northern component is compact (core) Preston et al. 1989
  • similar structure as Preston et al. 1989 (better resolution): two components aligned in SE separation 35mas Shen et al. 1998
  • core elongated to E - SE with a separation of 1mas (Tingay et al. 2002)

• 0454-463

  • core-dominant, flat spectrum radio source (flux 2.06 Jy at 5 GHz) (Kühr et al. 1981)
  • highly polarized quasar, measurements of 7.2% (Impey & Tapia 1990) to 27.1% (Wills et al. 1992)
  • compact core, no additional components visible (Ojha et al. 2004)
  • source detected with EGRET (Thompson et al. 1993, Hartman et al. 1999)

• 0506-612

  • note on NED: blazar (z = 1.093) with a strong associated metal absorber at z = 1.079 (Bechtold et al. 2002)
  • strong COMPTEL (1-10 MeV) source in the region close to the source, but only very weak EGRET source (above 100 MeV, 3 sigma source) (Bloemen et al. 1995)
  • compact core Ojha et al. 2004

• 0518-458

  • PICTOR A is one of the very few nearby (z=0.035) FR II-type radio galaxies (Fanaroff & Riley 1974)
  • FRII broad-line radio galaxy with a strong double-lobed radio source oriented along the east-west direction (Christiansen et al. 1977)
  • extended X-ray emission coincident with the eastern radio lobe (most likely non-thermal mechanism) Grandi et al. 2003
  • VLBI maps: jet to the west, apparent motions for three of the five parsec-scale jet components have been estimated: 0.5 +/- 0.4 c, 1.1 +/- 0.5 c and 0.4 +/- 0.7 c, no parsec-scale counterjet has been detected (Tingay et al. 2000)
  • double peaked Balmer line component (torus model) Halpern et al. 1994
  • Chandra observation: X-ray emission is detected from the nucleus, a 1.''9 (110 kpc) long jet to the west of the nucleus, the western radio hot spot some 4.''2 (240 kpc) from the nucleus, and the eastern radio lobe Wilson et al. 2001
  • counterjet????

• 0521-365

  • (z = 0.055, Bolton et al. 1965) BL Lac with strong H I emission lines, intense broad permitted lines have appeared in the spectrum (Ulrich et al. 1981)
  • blazar, powerful radio source, remarkable for its optical synchrotron jet (Danziger et al. 1979; Boisson, Cayatte, & Sol 1989, Scarpa et al. 1999)
  • exhibits strong broad and variable nuclear optical emission lines (Scarpa, Falomo, & Pian 1995)
  • map: core jet northwestward consisting of a core and two additional components separated from the core by 3.38 and 8.27 mas (Shen et al. 1998)
  • map: core and component to NW with 3mas separation (Ojha et al. 2004)
  • (Tingay et al. 2002 b)
  • NED note: object contains a well-studied optical/radio jet extending to the northwest (see Scarpa et al. 1999b and references therein), which was recently detected in the X-rays (Birkinshaw, Worrall, & Hardcastle 2002) (Cheung at al. 2003)

• 0537-441

  • BL Lac (z = 0.894), candidate for a gravitational lens ( Stickel, Fried, & Kuhr 1988; Romero, Surpi, & Vucetich 1995) disputed by other authors (Falomo, Melnick, & Tanzi 1992; Lewis & Williams 1997)
  • strong variable EGRET gamma-ray source (Thompson, Bertsch, & Fichtel 1993, Hartman et al. 1999)
  • source with a GPS-type spectrum, with spectral peak at 5 GHz (Tornikoski et al. 2001)
  • VLA map: curved jet-like structure leading to the west (Cassaro et al. 1999)

• 0625-354

  • VLBA map: "core-jet" structure, faint component to the southeast of the core is in the direction of the larger-scale jet. correlation position was 22" north of the core position, image may have some distortion (Fomalont et al. 2000)
  • NED note: optical counterpart of this FRI radio source, located at the center of the cluster Abell 3392, is a giant elliptical embedded in a rich environment. It is worth noticing the presence of a strong point source in the nucleus of this galaxy (Govoni et al. 2000)

• 0637-752

  • peculiar emission line at 1.60+/-0.07 keV and equivalent width 59^+38_-34 eV (both in the quasar frame) in the X-ray spectrum of this radio-loud quasar (Yaqoob et al. 1998)
  • VLBI map: component to the west (separation ~5mas) (Ojha et al. 2004)
  • map: component to the west (separation ~1.5mas) (Tingay et al. 2002)
  • first celestial Chandra target, 100 kiloparsec X-Ray Jet discovered by Chandra, coinciding with optical and radio contours (Tingay at al. 1998), jet to west turning to the northwest after ~10 as and a single hot spot to the east of the core (Schwartz et al. 2000)
  • Chandra observation: at least 4 knots in the jet resolved, separated from the core by a few arcseconds (Chartas et al. 2000)
  • apparent superluminal speed of this jet on the parsec-scale, SSC model of an electron-positron jet with a Doppler factor of ~10 (Edwards et al. 2006)
  • proper motions are just consistent with a weighted average apparent speed of (17.8 +/- 1.0)c (H_0 = 70 km/s and q_0 = 0.15; Schwartz et al. 2000; Lovell et al. 2000b)

• 1104-445

  • map: first southern VLBI compact shows core with additional component ~17mas ENE (Preston et al. 1989)
  • map: slight (?) jet curvature at ~1.8 mas from the northeast to the north (Shen et al. 1997)
  • map: structure in NE direction, core heavily resolved (Tingay et al. 2002)

• 1144-379

  • BL Lac object, optical, infrared and rapid radio variability, featureless powerlaw spectrum (Nicolson et al. 1979)
  • first VLBI map: unresolved core (Shen et al. 1997)

• 1257-326

  • flat-spectrum, radio-loud quasar, extreme IDV source, Rapid Interstellar Scintillation (Bignall et al. 2003)
  • for ISS: upper limit on the distance to the scattering plasma of no more than 10 pc (Bignall et al. 2006)

• 1313-333

  • possible EGRET detection of this flat spectrum QSO (Nolan et al. 1996)
  • map: jet components to the west, separated from the core by a few mas (4.7 at 2.32 GHZ, and 0.9 and 4.5 mas at 8.55 GHz) (Fey et al. 1996)
  • source is very variable at the high radio frequencies, EGRET detections have been made at the increase of millimeter-wave activity, from the end of 1991 to the first half of 1993. The radio spectrum is extremely flat, likely counterpart of 3EG J1313-431 (Tornikoski et al. 2002)

• 1322-428

  • Centaurus A

• 1323-526

  • IDV source (McCulloch et al. 2005)
  • Bignall et al. 2008 suggest a tentative association of this little-studied IDV flat-spectrum radio source with the unidentified EGRET source 3EG J1316-5244

• 1333-337

  • large scale jet: 2 outer components separated by 30 arcmin (650 kpc) and two inner components separated by 2 arcmin (45 kpc) (Goss et al. 1977)
  • NED note by Jones et al. 1992: strong slightly-bent bridge or jet between two diffuse lobes. The bridge shows double structure (inner lobes) near the centre, but not a distinct core. The lobes are edge-brightened although it is an intrinsically weak radio source. Mapped by Gardner & Whiteoak (1971), SM, Goss et al. (1977), Slee (1977), Swarup (1984), Killeen et al. (1986) and Ekers et al. (1989)
  • NED note by Govoni et al. 2000: regular elliptical galaxy located at the center of cluster Abell 3565 (it is the brightest one)
  • NED note by Jensen et al. 2001: compact dust ring close to the nucleus
  • on the parsec scale, a jet and a counterjet (direction NW,SE) extend out from a central unresolved core in the 8.4 GHz image, which is consistent with the large scale jet, pointlike emission from center of the galaxy, bolometric luminosity of the unresolved source: 2*10^{-5} of the Eddington luminosity of a 10^9 solar mass BH, thermal soft X-ray emission frum the nucleus with a broader radial profile than the PSF (from hot gas ~0.56 eV), northwestern jet is brighter (Doppler boosting in an intrinsically symmetric source), relativistic bulk speed (0.79c) (Pellegrini et al. 2003, analysis with VLBA and Chandra)

• 1424-418

  • NED note by Shen et al. 1998: highly optically polarized quasar (Impey & Tapia 1988, 1990), z=1.524, VLBI image shows two components separated by ~3 mas. Assuming the stronger component is the core, the position angle of the weaker component is 260^deg^, significantly different from the reported value for the two 2.3 GHz components of 236^deg^/284^deg^ (Preston et al. 1989)
  • NED note: jet extending 1" to the west of a compact core (Marshall et al. 2005)
  • map: unresolved core, no additional components (Ojha et al. 2004)
  • map: core slightly extended to the east (Tingay et al. 2002)

• 1454-354

  • Fermi/LAT discovery of gamma-ray emission from the flat-spectrum radio quasar PKS 1454-354 (Fermi/LAT collaboration 2009)
  • indication for weak EGRET detection, PKS 1454-354 and PKS 1501-343 are possible counterparts of the EGRET source 3EG J1500-3509 (Mattox et al. 2001, Sowards-Emmerd et al. 2004)

• 1501-343

  • Mattox et al. 2001 and Sowards-Emmerd et al. 2004 list this source and 1454-354 as a possible counterpart for the EGRET source 3EG J1500-3509
  • Petrov et al. 2007 did not detect this source at 22 GHZ in six observations with a minimum flux density limit of 170 mJy.

• 1549-790

  • NED note: core-jet radio source of ~400 pc [about 120 milliarcsec (mas)] in size and has been studied in detail at radio frequencies by King (1994) and King et al. (1996) using the southern VLBI network, the [O III]lambda5007 has one of the largest widths measured in radio galaxies (Morganti et al. 2001)
  • NED note: radio jets are pointing close to our line of sight (Tadhunter et al. 2001)
  • Holt et al. 2006: luminous quasar observed at an early stage of its evolution, quasar and jet activity have been triggered in a major merger which has also triggered substantial star formation, accreting at close to the Eddington rate, the black hole in this system is growing rapidly and simultaneously driving relativistic jets, links together several classes of active galaxies, common properties with high-redshift AGN
  • map: two components (core and one comp. SW, separation ~4mas) (Ojha et al. 2005)

• 1610-771

  • strong flat spectrum radio source identified with a QSO, steep power law continuum (nu^{-3.8}, atmosph. correction: nu^{-2.7}), until then highest redshift (z=1.71) QSO with steep optical continuum (Hunstead et al. 1980)
  • strongly curved spectrum indicating a strong ultraviolet absorption by dust (Courbin et al. 1997)
  • map: modeled as 3.8 Jy component 10 mas in extend with a 1.4 Jy halo approximately 50 mas in diameter (data with 22 mas resolution) (Preston et al. 1989)
  • map: presence of extended component, small scale structure: 3 components at a position angle of -30 degree within about 3 mas (southern one is the brightest one, but not necessarily the core) (Tingay et al. 2002)
  • map: 3 components in the E-W line, separated by 40mas each (Ojha et al. 2005)

• 1714-336

  • possible counterpart of 3EG J1718-3313 (Sowards-Emmerd et al. 2004)

• 1716-771

  • possible counterpart of 3EG J1720-7820, only one 90 GHz data point, very faint source (S/N less than 4), upper limit 370 Jy at 90 GHZ (Tornikoski et al. 2002)

• 1718-649

  • NGC 6328, closest (z = 0.014) gigahertz-peaked spectrum radio galaxy (closest and best studied GPS source), suggestion that GPS sources arise as a consequence of galaxy merger activity (NGC 6328) (Tingay et al. 1997)
  • one of the closest GPS sources (distance: 56 Mpc), closer PGS sources are: NGC 1052 (18 Mpc) and IC 1459 (PKS B2254-367, 19 Mpc) (Tingay et al. 2003)
  • the object is regarded as a merger of two galaxies, at least one of which is a gas-rich spiral, in the process of forming an elliptical. (Fanti et al. 2000)
  • analysis of radio spectrum and variability of this source: synchrotron self-absorption or free-free absorption as the sole process responsible for the gigahertz-peaked spectrum (Tingay & Kool 2003)

• 1733-565

  • NED note by Govoni et al. 2000: FRII radio source (Morganti et al. 1993), with emission lines in the optical spectrum (Simpson et al. 1996)
  • map: unresolved core, tiny component SW separation ~10mas (Ojha et al. 2004)
  • in the kpc-scale: extended lobes, bridge and core emission. radio-lobes (in the SW and NE) separated by 4.57 arcmin (Hunstead et al. 1982)
  • SPIRAL observations: emission-line gas is measured to be rotating about and extended perpendicular to the (kpc-scale) radio axis (Bryant & Hunstead 2002)

• 1759-396

  • indentified with the source 3EG J1800-3955 (Sowards-Emmerd et al. 2004)
  • indentified with 2EG J1800-4005 with 81% confidence (Mattox et al. 1997)

• 1804-502

  • possible counterpart of 3EG J1806-5005, only one 90 GHz data point, very faint source (S/N less than 4), upper limit 250 Jy at 90 GHZ (Tornikoski et al. 2002)

• 1814-637

  • compact steep-spectrum (CSS) source with a basic double-lobed structure oriented almost north-south, no information which structures (if any) correspond to the core, (Tzioumis et al. 1996, Tzioumis et al. 2002)
  • redshift z=0.645 determined, problematic due to bright foreground star (Morganti et al. 2001)
  • map: two components, separated by ~90mas, NNW (Ojha et al. 2004)
  • map: two (resolved) components, one 200-300mas to the south, problably an additional small component in between (Tzioumis et al. 2002)

• 1933-400

  • identified with the source 3EG J1935-4022 (Hartman et al. 1999)
  • VLA observation: diffuse secondary extending from core to r = 3.5 arcsec in p.a. 140 degree (Perley 1982)

• 1934-638

  • one of the earliest known GPS sources (Kellermann 1966, Bolton et al. 1963)
  • VLBI imaging reveals the GPS source has a compact double morphology with a separation of 42 mas orientated east-west (Tzioumis et al. 1989, 1998)
  • this GPS radio galaxy is significantly polarized in the UV with the polarization E-vector close to perpendicular to the radio axis (Tadhunter et al. 2002)
  • Compton thick source (shown by BeppoSAX observations), high equivalent width of Fe K alpha line (EW greater 1keV) (Risaliti et al. 2003)
  • map: two components, separated in E-W direction by ~40mas (Ojha et al. 2004)

• 1954-388

  • optically violent variable (Gilmore 1980)
  • high optical polarization, up to 11% (Impey & Tapia 1988, 1990)
  • VLBI observations showed the presence of a compact core at 2.3 GHz (Preston et al. 1985)
  • VLBI image shows a single compact component 0.4 mas x 0.3 mas in size, with a flux density of 1.9 Jy (Shen et al. 1998)
  • noted as a new source with a GPS-type spectrum by Tornikoski et al. (2001), with turnover at ~10 GHz, the compilation of data would suggest that the spectral peak lies closer to 8 GHz (Edwards & Tingay 2004).
  • a compact core-jet morphology (core elongated to the SSE) was revealed by the VLBA observations of Fomalont et al. (2000)
  • map: compact core (tiny component ~3mas to the west) (Ojha et al. 2004)

• 2005-489

  • one of the brightest known BL Lac sources (Wall et al. 1986)
  • Discovery of VHE gamma rays, the first AGN independently discovered by HESS as an emitter of VHE photons and only the second such AGN known in the Southern Hemisphere, the softest VHE spectrum (Gamma = 4.0) ever measured from a BL Lac (Aharonian et al. 2005)
  • classified as a high-frequency peaked BL Lac (HBL) due to its X-ray-to-radio flux ratio (Sambruna et al. 1995)
  • source detected with EGRET (Lin et al. 1999)
  • map: unresolved core, additional component to the SW with separation ~3mas (Ojha et al. 2005)
  • map: compact core (Shen et al. 1998)

• 2027-308

  • NED note: probably a member of the class of very-narrow-line emission galaxies (Grandi 1983)
  • possible counterpart for 3EG 2034-3110 (Sowards-Emmerd et al. 2004)

• 2052-474

  • quasar (z = 1.489) has a bright radio core and a two-sided arcsec-scale radio jet. VLBA data on this object have not revealed the presence of a milliarcsec-scale jet (Tingay et al. 1998). We detect no extended X-ray emission. (Chandra) (Marshall et al. 2005)
  • identified with the EGRET source 3EG J2055-4716 (Hartman et al. 1999)
  • map: compact core (Ojha et al. 2004)

• 2106-413

  • NED note by Kollgaard et al. 1995: This object has been identified as a quasar at z = 1.055 with several emission lines with equivalent widths of 27-55 A (White et al. 1988). The radio core is moderately polarized (3.5%; Impey & Tapia 1990). Our ATCA observations show the radio spectrum rises at low frequencies with {alpha} = +0.2, peaking near 5 GHz. However, with C = 0.8, the spectral energy distribution is not strongly inverted
  • core slightly resolved in the VLBA image (Fomalont et al. 2000)

• 2149-306

  • high-redshift, high-luminosity, radio-loud quasar with a strongly blueshifted Fe K alpha line (at ~17 keV in the quasar frame) (Yaqoob et al. 1999, Wang et al. 2003)
  • blueshifted lines due to extremely large outflow bulk velocities of 0.6c-0.75c (Basu 2006)
  • object hosts a bright X-ray source extensively observed in the past by ROSAT and ASCA (Siebert et al. 1996; Cappi et al. 1997), BeppoSAX (Elvis et al. 2000), Chandra (Fang et al. 2001), XMM-Newton (Ferrero & Brinkmann 2003), and more recently by Swift (Sambruna et al. 2007)
  • map: core and component to the W, separation 8.7 mas (Ojha et al. 2005)

• 2152-699

  • NED note: Fosbury et al. (1990) suggest that this radio galaxy is a blazar. The radio structure shows a core, a nearby bright lobe and a more distant diffuse lobe; in the true definition of Fanaroff & Riley, an FR II. There is a bright extended emission-line blob to the north-east of the core. (Morganti et al. 1993)
  • one of the brightest sources in the sky at 2.3 GHz (Wall et al. 1994)
  • image of kpc-scale radio structure shows the classic double-lobed structure of FR-II type radio sources (Fosbury et al. 1990)
  • parsec-scale radio jet aligns strongly with optical emission line features, and not with the kiloparsec-scale radio structure (Tingay et al. 1996)
  • (Young et al. 2005)
  • a system of low-ionization filaments extending out to a maximum radius of 20 arcsec and, to the north-east, a luminous cloud at a distance of 10 arcsec from the nucleus. In addition to emission lines of extremely high ionization, the cloud has a continuum that is considerably bluer than that of the underlying stellar population. The radial ionization gradient noted suggests that the nucleus provides the ionizing energy for the cloud, and the tangential ionization gradient suggests that this energy is directed toward it in an intense radiation or plasma beam. radio axis and optical emission line features on the kiloparsec-scale appear to have an obvious connection but are somewhat misaligned (most likely being due to an interaction between the radio jet and an extra-nuclear cloud of gas, the misalignment possibly caused by the deflection of the radio jet in the interaction) (Tadhunter et al. 1988)
  • map: VSOP image shows a resolved core and highly linear, narrow jet approximately 6 mas in extent to the NE (Tingay et al. 2002)
  • map: core with additional jet component to the NE, separation a few mas (Ojha et al. 2004)

• 2155-304

  • NED note: typical X-ray-selected BL Lac object and one of the TeV {gamma}-ray sources (Griffiths, Briel, & Chaisson 1979). This source is one of the brightest and the most intensively studied object of this class (see Smith et al. 1992; Treves et al. 1989) (Xie et al. 2001)
  • one of the brightest extragalactic X-ray sources in the sky and as a result other X-ray satellites, including ROSAT, BeppoSAX, RXTE, and Chandra (Brinkmann et al. 1994, Chiappetti & Torroni 1997, Vestrand & Sreekumar 1999, Nicastro et al. 2002)
  • compact, flat-spectrum radio source (~300 mJy?), and exhibits an essentially featureless continuum from radio to X-ray frequencies, maximum power emitted by PKS 2155-304 is between the UV and soft X-ray range, and it is the brightest BL Lac detected in the UV regime (Wandel & Urry 1991)
  • detected by EGRET (Vestrand et al. 1995)
  • VHE gamma-rays from this source were observe (Aharonian et al. 2005)
  • TeV flare observered (July 2006) (Aharonian et al. 2007)
  • map: only compact core without additional components (Ojha et al. 2004)
  • measured apparent speed of the single jet component was 0:93c +/- 0:31c (Piner et al. 2008)

• 2204-540

  • QSO with a flux of 1.3 Jy at 18.5 GHz with a polarization of 6.6 +/- 0.2 % (Ricci et al. 2004)

• 2326-477

  • Scott et al. 2004 find a compact, unresolved core structure smaller than 0.1 mas^2 of 410 mJy and a brightness temperature above 3*10^11 K at 5 GHz.
  • Tingay et al. 2003 find a substantially higher mean flux-density 5 GHz of 1.63 Jy with ATCA and a moderate variability index of 0.05, suggesting that a substantial fraction of the 5 GHz total brightness is emitted on larger scales unresolved for the space-VLBI array.
  • our image shows jet-like emission peaking in two distinct components ~6 mas to the east and ~10 mas to the north-east of the compact core at 8.4 GHz

• 2355-534

  • optically violent and highly polarized source (Impey & Tapia 1988, 1990)
  • image shows two components with similar size but different flux densities. The stronger component, which may be the core, has a brightness temperature of 3.5x10^11 K. The second component is located at a distance of 4.9 mas at a position angle of 235^deg (Shen et al. 1998)
  • the VSOP data proved insufficient to produce an image, single-component model fit of the data (Tingay et al. 2002)