High-resolution images for astro-ph/0606460

"The Connection Between Barstrength and Circumnuclear Dust Structure"

1. First Part (NGC0289--NGC3169)   postscript     gif
   Second Part (NGC3227--NGC5194)    postscript    gif
   Third Part (NGC5236--NGC7727)   postscript    gif
   Structure maps for 75 galaxies with measured barstrengths. Each panel shows the inner 5% of D₂₅ from the RC3 catalog. The solid white circles are given by a radius of r_c, as defined in eq. 3). In the case that r_eff(bulge) > r_c, the bulge radius is marked by a dashed white circle; these dashed circles were not included on the structure maps used for classification, but are merely given here for reference. Dark regions are dust, while bright regions are emission. Several images (e.g., NGC2997) also include the ACS coronographic finger. North is up and east is to the left.
   
   
2. Prototypes   postscript   gif
   Structure maps of prototypes for the six circumnuclear morphology classes.
   
   
3. Degraded NGC4321   postscript   gif
   Degraded structure maps of NGC4321 for testing the dependence of structure map rms  σ_sm on resolution. The percents in the upper lefthand corners are the percent change in σ_sm relative to the original structure map. The numbers in the upper right-hand corners are the standard deviations in pixels of the Gaussians with which both the image and the PSF were convolved before making the structure map. The white circles are given by a radius of r_c, as defined in eq. 3. The resolution of the original image is 0.06'', or 4.9 pc, while the resolution of the 2.6-σ Gaussian convolved image is 0.13'', or 10.8 pc. This is equivalent to moving the galaxy from 16.8 Mpc to 37 Mpc. Relative to the measured uncertainty on the original σ_sm is 2.1%, there is essentially no change in σ_sm with resolution.
   
   
4. Q_b: TW v. others    postscript   gif
   Comparison of Q_b for TW galaxies and all other galaxies. The vertical spreads correspond to the central 68 percentile spread of the cumulative fraction and are due to the uncertainty in Q_b. Galaxies with TW circumnuclear dust spirals are more weakly barred than typical galaxies, with a 2% probability of being drawn from the same parent distribution.
   
   
5. Left Panel: T type distribution     postscript    gif
   Right Panel:  T≥6    postscript     gif
   Left: No connection is seen between Hubble T-type for T≤5 and nuclear classification. Right: Structure maps for the four galaxies in the sample with T≥6. The large scale morphologies from the RC3 catalog are: NGC3077, I0; NGC4504, Scd; NGC1385, Scd; NGC4027, Sdm. All four of these galaxies are classified as having chaotic circumnuclear dust structure.
   
   
6. Left Panel: Q_b distribution, histogram           postscript     gif
   Right Panel: Q_b distribution, cumulative fractions    postscript     gif
   Nuclear classifications and barstrength Q_b. Left: Distribution of nuclear classification into different barstrength classes. Right: Monte Carlo average cumulative distribution of barstrength in each nuclear class and total sample.
   
   
7. LGD at larger scales, not at small:
   NGC1530    postscript    gif
   NGC2964    postscript    gif
   NGC4314    postscript    gif
   NGC6300    postscript    gif
   Four examples of galaxies with LGD (large grand design) but not SGD (small grand design) structure. Left: Width and height are given by 0.1D₂₅. Right: Width and height are given by r_c. The classifications are: NGC1530, TW; NGC4314, LW; NGC6300, CS; NGC2964, C. The white circles in both panels have radius r_c. Dark regions are dust, while bright regions are emission. North is up and east is to the left
   
   
8. Left Panel: LGD v. SGD, Q_b      postscript    gif
   Left Panel: LGD v. SGD, σ_sm      postscript    gif
   Comparisons of barstrengths Q_b and structure map rms σ_sm for SGD and LGD galaxies. The vertical widths correspond to the central 68-percentile spread of the cumulative fraction and are due to the uncertainty in Q_b and σ_sm. SGD galaxies are less strongly barred (left) and have less dust structure (right) than LGD galaxies. There is a 0.4% probability that the Q_b are drawn from the same parent population, and 3% probability that the rms values are drawn from the same parent distribution.
   
   
9. Ring v. No ring, Q_b      postscript    gif
   Comparison of Q_b for LW galaxies with and without circumnuclear rings. The vertical widths correspond to the central 68-percentile spread of the cumulative fraction and are due to the uncertainty in Q_b. Galaxies with circumnuclear rings are found to be more strongly barred than typical galaxies, with 1.5% probability of being drawn from the same parent population.
   
   
10. Circumnuclear rings      postscript    gif
    Structure maps of the eight galaxies in our sample with circumnuclear rings in order of increasing Q_b. All eight have LGD structure. Width and height are given by 0.1D₂₅.
    
    
11. Strongly Barred Galaxies      postscript    gif
    Structure maps for the 12 most strongly barred galaxies in our sample (Q_b≥4). Q_b increases to the right and then down. These galaxies have LGD structure (NGC1300, NGC1365, NGC5643, NGC4314, and NGC1530), chaotic nuclear structure (NGC6221, NGC3359, NGC1073, NGC4027, and NGC7479), or a chaotic nuclear spiral (NGC0613 and NGC2442). Two of the LGD spirals are associated with a circumnuclear ring (NGC1300 and NGC4314). Dark regions are dust; bright regions are emission.
    
    
12. SB comparison of σ_sm       postscript    gif
    Comparisons of structure map rms σ_sm of SB galaxies. The vertical spreads correspond to the central 68-percentile spread of the cumulative fraction and are due to the uncertainty in Q_b. SB(r) galaxies have less dust structure than SB(rs) galaxies, which, in turn, have less dust than SB(s) galaxies. Specifically, with ≥99% confidence, SB(r) galaxies have less central dust structure than SB(s) galaxies.