Sasmirala Individual Information for NGC 985
Description
NGC 985 is a peculiar ring-like late-stage merger system, at a redshift of z = 0.0431 (D ~ 195 Mpc). The two nuclei have a separation of 3.5arcsec (~ 3 kpc; PA~ 110∘; [appleton_infrared_1993]). The eastern nucleus is classified a Sy 1.5 [veron-cetty_catalogue_2010], belonging to the nine-month BAT AGN sample. After IRAS, N-band photometry with MMT [maiolino_new_1995] and MIR imaging with ISO [appleton_mid-infrared_2002] was obtained. NGC 985 was also observed with Spitzer/IRAC and IRS, and both nuclei are blended in the IRAC images, resulting in a slightly elongated compact MIR source with part of the ring-like host structure also visible. The IRS LR staring-mode spectrum exhibits possibly weak silicate 10 and 18 μm emission, PAH emission and an emission peak at ~ 17 μm (see also [mullaney_defining_2011]). NGC 985 was observed with VISIR in five N-band filters in 2008 (unpublished, to our knowledge), and only one unresolved nucleus was detected in all images but B9.7, where the nucleus appears slightly extended. The nuclear VISIR photometry is consistent with the Spitzer spectrophotometry, which indicates that the AGN dominates the MIR emission in the central 3 kpc of NGC 985.
- [appleton_infrared_1993] P. N. Appleton and P. M. Marcum. Infrared observations of the seyfert ring galaxy NGC 985 . ApJ , 417 pp. 90, November 1993.
- [appleton_mid-infrared_2002] P. N. Appleton, V. Charmandaris, Yu Gao, F. Combes, F. Ghigo, C. Horellou, and I. F. Mirabel. Mid-infrared and CO observations of the Infrared/X-Ray luminous seyfert 1 galaxy NGC 985: The making or breaking of a ULIRG? . ApJ , 566 pp. 682–698, February 2002.
- [maiolino_new_1995] R. Maiolino, M. Ruiz, G. H. Rieke, and L. D. Keller. New constraints on the unified model of seyfert galaxies . ApJ , 446 pp. 561, June 1995.
- [mullaney_defining_2011] J. R. Mullaney, D. M. Alexander, A. D. Goulding, and R. C. Hickox. Defining the intrinsic AGN infrared spectral energy distribution and measuring its contribution to the infrared output of composite galaxies . MNRAS , page 474, April 2011.
- [veron-cetty_catalogue_2010] M.-P. Véron-Cetty and P. Véron. A catalogue of quasars and active nuclei: 13th edition . A&A , 518 pp. 10, July 2010.
Images
Optical image (DSS, red filter). Displayed are the central 4 arcmin with North being up and East to the left. The colour scaling is linear with white corresponding to the median background (BG) and black to the 0.01% pixels with the highest intensity.
Spitzer MIR images. Displayed are the inner 40 arcsec with North being up and East to the left. The colour scaling is logarithmic with white corresponding to median BG and black to the 0.1% pixels with the highest intensity. The label in the bottom left states instrument and central wavelength of the filter in micron (I: IRAC, M: MIPS).
Subarcsecond-resolution MIR images sorted by increasing filter central wavelength. Displayed are the inner 4 arcsec with North being up and East to the left. The colour scaling is logarithmic with white corresponding to median BG and black to the 75% of the highest intensity of all images in units of sig_bg. The inset image (where present; either bottom or top right) shows the central arcsecond of the PSF from the calibrator star, scaled to match the science target. The labels in the bottom left state instrument and filter names (C: COMICS, M: Michelle, T: T-ReCS, V: VISIR).
SEDs
MIR SED. The description of the symbols in all the SED plots (where present) is the following: Grey crosses and solid lines mark the Spitzer/IRAC, MIPS and IRS data. The colour coding of the other symbols is as follows: green for COMICS, magenta for Michelle, blue for T-ReCS and red for VISIR data. Darker-coloured solid lines mark spectra of the corresponding instrument. The black filled circles mark the nuclear 12 and 18 micron continuum emission estimate from the data (where present). The ticks on the top axis mark positions of common MIR emission lines, while the light grey horizontal bars mark wavelength ranges affected by the silicate 10 and 18 micron features.