Sasmirala Individual Information for Ark 120
Description
Ark 120 is a spiral galaxy at a redshift of z = 0.0327 (D ~ 149 Mpc) hosting a radio-quiet Sy 1 nucleus [veron-cetty_catalogue_2010] that belongs to the nine-month BAT AGN sample. The NLR morphology appears halo-like [mulchaey_emission-line_1996]. The first ground-based N- and Q-band photometry of the nucleus were obtained with IRTF in 1983 and UKIRT in 1984 [ward_continuum_1987]. After IRAS, MIR observations were carried out with ISO/ISOCAM [ramos_almeida_mid-infrared_2007] and Spitzer/IRAC, IRS and MIPS, where Ark 120 appears as an unresolved nucleus without any further host emission being detected. The IRS LR staring-mode spectrum shows strong silicate emission, PAH emission and a blue spectral slope in νFν-space (see also [sargsyan_infrared_2011]). The nucleus of Ark 120 was observed with VISIR in 2009 and 2010 in a total of five N-band filter images. An unresolved nucleus without further host emission was detected in all cases. The corresponding nuclear fluxes of the three 2009 measurements match the Spitzer spectrophotometry, while the 2010 measurements are ~ 20% lower for unknown reasons.
- [mulchaey_emission-line_1996] John S. Mulchaey, Andrew S. Wilson, and Zlatan Tsvetanov. An emission-line imaging survey of early-type seyfert galaxies. i. the observations . ApJS , 102 pp. 309, February 1996.
- [ramos_almeida_mid-infrared_2007] C. Ramos Almeida, A. M. Pérez García, J. A. Acosta-Pulido, and J. M. Rodríguez Espinosa. The mid-infrared emission of seyfert galaxies: A new analysis of ISOCAM data . AJ , 134 pp. 2006–2019, November 2007.
- [sargsyan_infrared_2011] Lusine Sargsyan, Daniel Weedman, Vianney Lebouteiller, James Houck, Donald Barry, Ashot Hovhannisyan, and Areg Mickaelian. Infrared spectra and spectral energy distributions for dusty starbursts and active galactic nuclei . ApJ , 730 pp. 19, March 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.
- [ward_continuum_1987] Martin Ward, Martin Elvis, G. Fabbiano, N. P. Carleton, S. P. Willner, and A. Lawrence. The continuum of type 1 seyfert galaxies. i - a single form modified by the effects of dust . ApJ , 315 pp. 74–91, April 1987.
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.