Sasmirala Individual Information for NGC 4151

Description

NGC 4151 is a nearly face-on barred spiral galaxy at a distance of D = 13.3 ± 1 Mpc [mundell_nuclear_2003] with a Sy 1.5 nucleus [veron-cetty_catalogue_2010]. This galaxy is one of the original six Seyfert galaxies [seyfert_nuclear_1943] and host the flux-brightest, nearest and most variable type I AGN. Therefore, it belongs to the best-studied AGN at all wavelengths (see [ulrich_active_2000] for a review). NGC 4151 also belongs to the nine-month BAT AGN sample. The AGN is surrounded by an extended biconical NLR with an inner extent of ~ 5.5arcsec ~ 350 pc along a PA~ 67^∘ ( e.g., [pogge_circumnuclear_1989, perez_complex_1989, evans_hubble_1993]). This roughly coincides with a two-sided radio outflow with total extent of ~ 600 pc along a PA~ 77^∘ [wilson_radio_1982] and a collimated jet in the central ~ 100 pc [mundell_nuclear_2003]. In addition, nuclear water maser emission was detected in this object [braatz_green_2004, tarchi_new_2011]. Pioneering MIR observations of NGC 4151 were performed by [low_proceedings_1968]. Early follow-up observations by [stein_possible_1969], [kleinmann_observations_1970] and [rieke_variability_1972] found apparent N-band flux variations of a factor of a few over the course of three years. However, later measurements constrained possible N-band flux variations to \⪅20% [stein_observations_1974, rieke_infrared_1978, lebofsky_extinction_1979, rieke_spectral_1981, ward_continuum_1987]. The first N-band spectrum was presented by [jones_dust_1984], followed by [aitken_8-13_1985] and [roche_atlas_1991], while [neugebauer_size_1990] made a first attempt to measure the size of the MIR nucleus in NGC 4151 with bolometer-based scanning method. Its emission was also studied with ISO [rodriguez_espinosa_bimodal_1996, sturm_infrared_1999, alexander_infrared_1999, rigopoulou_large_1999]. The first subarcsecond-resolution MIR images were obtained in 2000 with Palomar 5 m/MIRLIN [gorjian_10_2004] and Keck/LWS [soifer_high_2003], and in 2001 with Gemini/OSCIR [radomski_resolved_2003]. The images show a dominating unresolved MIR nucleus, while the OSCIR images also reveal extended emission (~ 3.5arcsec ~ 220 pc) coinciding with the NLR (PA~ 60^∘). NGC 4151 was also observed with Spitzer/IRAC, IRS and MIPS, and the corresponding images are completely dominated by the bright nucleus outshining the spiral-like host emission. The IRAC 5.8 and 8.0 μm PBCD images are saturated and thus not analysed (but see [gallimore_infrared_2010]). The IRS LR staring-mode spectrum exhibits silicate 10 and 18 μm emission, very weak PAH features and an emission peak at ~ 18 μm in νF_ν-space (see also [weedman_mid-infrared_2005, buchanan_spitzer_2006, wu_spitzer/irs_2009, deo_mid-infrared_2009, gallimore_infrared_2010]). Thus, the arcsecond-scale MIR SED appears AGN-dominated without significant star formation contribution. The nuclear region of NGC 4151 was imaged with Michelle in the Si-5 filter in 2007 (unpublished, to our knowledge), and with VISIR in the PAH1 and PAH2_2 filter 2009 and 2010 [kishimoto_mapping_2011]. In addition, a Michelle LR N-band spectrum was obtained in 2007 [alonso-herrero_torus_2011, esquej_nuclear_2014]. Owing to the high airmass, the nucleus appears elongated in the VISIR images similar to the corresponding standard star images. Therefore, the VISIR images cannot be used to investigate the source morphology. In the Michelle image, the nucleus appears marginally resolved (FWHM ~ 0.5arcsec ~ 32 pc), while the extended NLR-associated emission seen in the OSCIR image is not visible. At least a second epoch of deep low-airmass MIR subarcsecond imaging is required to verify the source morphology. Our nuclear photometry is consistent with [kishimoto_mapping_2011] and the Michelle spectrum, at least at longer wavelengths. The fluxes are on average ~ 22% lower than the Spitzer spectrophotometry. Comparison with the previous MIR photometry constrains any possible flux variation to \⪅20% in the N-band but a more detailed analysis has to be conducted. Note the the nucleus of NGC 4151 is resolved interferometrically with MIDI, and a multi-component structure with a few-parsec size is found [burtscher_dust_2009, burtscher_diversity_2013, kishimoto_mapping_2011].

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• [wu_spitzer/irs_2009] Yanling Wu, Vassilis Charmandaris, Jiasheng Huang, Luigi Spinoglio, and Silvia Tommasin. Spitzer/IRS 5-35 μm low-resolution spectroscopy of the 12 μm seyfert sample . ApJ , 701 pp. 658–676, August 2009.

Images

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.