Sasmirala Individual Information for NGC 5273
Description
NGC 5273 is a lenticular galaxy at a distance of D = 15.3 ± 3.3 Mpc (NED redshift-independent median) hosting an AGN, that has been optically classified either as a Sy 1.5 or a Sy 1.9 (see discussion in [trippe_multi-wavelength_2010]). It features a slightly elongated compact radio source (PA~ 5∘; [ulvestad_radio_1984, nagar_radio_1999]) and a cospatial one-sided NLR cone ~ 1arcsec ~ 74 pc to the south (PA~ 180∘; [ferruit_hubble_2000]). The first ground-based MIR observations are reported in [maiolino_new_1995]. In addition, NGC 5273 was observed with ISO [clavel_2.5-11_2000, ramos_almeida_mid-infrared_2007] and Spitzer/IRAC, IRS and MIPS. The corresponding IRAC and MIPS images show a compact nucleus embedded within weak diffuse host emission. Our nuclear MIPS 24 μm photometry provides a flux consistent with [temi_spitzer_2009]. The IRS LR staring-mode spectrum suffers from a low S/N but indicates significant PAH emission and a red spectral slope in νFν-space. The arcsecond-scale MIR SED is thus significantly affected by star formation. Note that [oi_comparison_2010] detect PAH 3.3 μm emission in the central ~ 120 pc of NGC 5273. We observed the nuclear region of NGC 5273 with Michelle in two N-band filters in 2010 and detected a compact MIR nucleus without further host emission. The nucleus appears marginally resolved in both images (FWHM(major axis)~ 0.53arcsec ~ 40 pc; PA~ 90∘). However, the Si-5 image is affected by strong vertical stripe-like sky residuals, which make this result uncertain. We classify the nucleus as possibly extended at subarcsecond resolution in the MIR. Our nuclear Michelle photometry is on average ~ 33% lower than the Spitzer spectrophotometry. We can not exclude that the nuclear MIR SED (~ 40 pc) is still significantly affected by star formation.
- [clavel_2.5-11_2000] J. Clavel, B. Schulz, B. Altieri, P. Barr, P. Claes, A. Heras, K. Leech, L. Metcalfe, and A. Salama. 2.5-11 micron spectroscopy and imaging of AGNs. implication for unification schemes . A&A , 357 pp. 839–849, May 2000.
- [ferruit_hubble_2000] Pierre Ferruit, Andrew S. Wilson, and John Mulchaey. Hubble space telescope WFPC2 imaging of a sample of early-type seyfert galaxies . ApJS , 128 pp. 139–169, May 2000.
- [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.
- [nagar_radio_1999] Neil M. Nagar, Andrew S. Wilson, John S. Mulchaey, and Jack F. Gallimore. Radio structures of seyfert galaxies. VIII. a distance- and magnitude-limited sample of early-type galaxies . ApJS , 120 pp. 209–245, February 1999.
- [oi_comparison_2010] Nagisa Oi, Masatoshi Imanishi, and Keisuke Imase. Comparison of AGN and nuclear starburst activity in seyfert 1 and 2 galaxies over a wide luminosity range based on near-infrared 2-4μm spectroscopy . PASJ , 62 pp. 1509, December 2010.
- [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.
- [temi_spitzer_2009] Pasquale Temi, Fabrizio Brighenti, and William G. Mathews. Spitzer observations of passive and star-forming early-type galaxies: An infrared color-color sequence . ApJ , 707 pp. 890–902, December 2009.
- [trippe_multi-wavelength_2010] M. L. Trippe, D. M. Crenshaw, R. P. Deo, M. Dietrich, S. B. Kraemer, S. E. Rafter, and T. J. Turner. A multi-wavelength study of the nature of type 1.8/1.9 seyfert galaxies . ApJ , 725 pp. 1749–1767, December 2010.
- [ulvestad_radio_1984] J. S. Ulvestad and A. S. Wilson. Radio structures of seyfert galaxies. VI - VLA observations of a nearby sample . ApJ , 285 pp. 439–452, October 1984.
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.