Galaxy Zoo Talk

NGC3507 1237668292834689151 AGZ000CZP0

  • zoob1172 by zoob1172

    NED notes:

    1. 2006ApJ...647..140F
      Re:NGC 3507
      This galaxy (L2, SBb) has two point sources in its central kiloparsec: one very
      faint (14 counts) close to the edge of the region and a central extended source
      embedded in a bright patch of diffuse emission. The central source had only 187
      counts, which did not allow us to test a wide variety of spectral models.
      Instead we estimated its luminosity by fitting a simple MEKAL model (the photon
      index of the best-fitting power-law model was unrealistic), and we find L_0.5-10
      keV = 1.2 x 10^39^ ergs s^-1^ after correcting for absorption. A weak, extended
      radio source (S_{nu}_ = 16 mJy) is detected at 1.45 GHz (Condon 1987), which
      suggests that this object is not an LLAGN. It could be a collection of supernova
      remnants producing a superbubble around it seen as the X-ray diffuse emission
      and radio extended source. The fact that the data could not be fitted with a
      realistic power-law index strengthens this idea. This indicates that the X-ray
      emission of this LINER is powered by stellar processes. This result is
      consistent with the estimate of the age of the stellar population, which
      indicates the presence of a young stellar component (10^6^ yr; Gonzalez Delgado
      et al. 2004).

    2. 2006A&A...460...45G
      Re:NGC 3507
      NGC 3507 (UGC 6123). No hard nuclear point source was detected for this galaxy
      (Fig. 5). The only previously published X-ray study is based on observations
      obtained with ASCA: Terashima et al. (2002) get {GAMMA} = 2.3 and N_H_ = 1.0
      x 10^22^ cm^-2^, but conclude that a power-law model ({GAMMA} = 1.7)
      describes the spectrum well.

    3. 2002ApJS..143...73E
      Re:NGC 3507
      NGC 3507.---SBb: Nuclear point source embedded in elliptical bulge.
      The bulge is threaded by a prominent bar. Grand-design two-armed
      spiral pattern, with the arms emerging at right angles to the ends of
      the bar. The arms are well defined, and generally smooth, although
      there are some knots in the inner arms. The arm emerging from the SE
      end of the bar is more tightly wrapped than that emerging from the NW
      end. The surface brightness of both arms drops abruptly after ~180deg.
      The arms can be traced through another ~180deg before they fade into
      the sky.


  • c_cld by c_cld

    My composite image of NGC3507 with HST data (HST Proposal 15323 by Jonelle Walsh Texas, A & M University)

    IDJA08010 WFC3 UVIS2-2K2C-SUB F475W

    IDJA08020 WFC3 UVIS2-2K2C-SUB F814W


    J110325.36+180807.3 1237668292834689151 ra, dec 165.855707113, 18.135373363 z(~) 0.003266 = 14.3 Mpc

    with foreground spectroscopic binary stars 1237668292834689150 at 133.8742 pc distance from earth measured by Gaia

    These two objects of similar magnitudes and angular separation of 22.7" elicit the perception of the depth of field by a 100k+ factor !