Jet- and Wind-driven Ionized Outflows in the Superbubble and Star-forming Disk of NGC 3079

By G. Cecil, Joss Bland-Hawthorn, Sylvain Veilleux, A. Filippenko. 2001

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Hubble Space Telescope WFPC2 images are presented that span the inner ~19 kpc diameter of the edge-on galaxy NGC 3079; they are combined with optical, emission-line imaging spectrophotometry and VLA images of radio polarization vectors and rotation measures. Ionized gas filaments within 9 kpc diameter project up to 3 kpc above the disk, with the brightest forming the ≈1 kpc diameter superbubble. They are often resolved into strands ≈0.″3 (25 pc) wide, which emerge from the nuclear CO ring as five distinct streams with large velocities and velocity dispersions (FWHM ≈ 450 km s-1). The brightest stream emits ≈10% of the superbubble Hα flux and extends for 250 pc along the axis of the VLBI radio jet to one corner of the base of the superbubble. The other four streams are not connected to the jet, instead curving up to the vertical ≈0.6 kpc above the galaxy disk, then dispersing as a spray of droplets each with ≈103 M☉ of ionized gas (the volume filling factor f > 3 × 10-3). Shredded clumps of disk gas form a similar structure in hydrodynamical models of a galaxy-scale wind. The pattern of magnetic fields and the gaseous kinematics also suggest that a wind of mechanical luminosity Lw ≈ 1043 ergs s-1 has stagnated in the galaxy disk at a radius of ~800 pc, has flared to larger radii with increasing height as the balancing interstellar medium pressure reduces above the disk, and has entrained dense clouds into a "mushroom vortex" above the disk. Hα emissivity of the filaments limits densities to ne > 4.3f-1/2 cm-3, hence kinetic energy and momentum to (0.4-5) × 1055 ergs and (1.6-6) × 1047 dyne s, respectively; the ranges result from uncertain space velocities. A prominent star-forming complex elsewhere in the galaxy shows a striking spray of linear filaments that extend for hundreds of parsecs to end in unresolved "bullets."

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b50ac93076056415bbe39cac22992a4049a88e5a

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THREE-DIMENSIONAL INTEGRAL FIELD OBSERVATIONS OF 10 GALACTIC WINDS. I. EXTENDED PHASE (≳10 Myr) OF MASS/ENERGY INJECTION BEFORE THE WIND BLOWS (2010, background): “…erg cm−2 s−1 arcsec−2 (cgs) for a plasma at 104 K. to a combination of several factors: (i) the emitting regions have a small filling factor (f < 1), (ii) some dust is mixed in with the filaments (cf. Cecil et al. 2001), and (iii) ξ < 1 for the AGN/starburst fraction of the bolometric luminosity.”
Kiloparsec-scale outflows are prevalent among luminous AGN: outflows and feedback in the context of the overall AGN population (2014, background): “…observed outflows as has been seen in local systems, where star-formation winds, nuclear winds (potentially AGN-driven) and radio jets all are playing a role (.g., Cecil et al. 2001; Storchi-Bergmann et al. 2010; Rupke & Veilleux 2011; also see discussion on our individual targets in Appendix A).”
Relativistic jet feedback – III. Feedback on gas discs (2018, background): “Cecil et al. (2001) model the bubbles as arising from the wide-angle mechanically driven nuclear outflow.”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, background): “The overall morphology is reminiscent of early simulations by Suchkov et al. (1994) of superwind structure, as well as radio observations of Cecil et al. (2001) who studied the coherence of the magnetic field inside similarly trailing lobes.”
THE MULTIPHASE STRUCTURE AND POWER SOURCES OF GALACTIC WINDS IN MAJOR MERGERS (2013, background): “For two different plausible values of n based on studies of other sources (2 and 3; see, e.g., Veilleux et al. 1994; Cecil et al. 2001), we list in Table 5 the best fit BSB parameters for the ionized gas in Mrk 273.”
A Survey of Kiloparsec-Scale Radio Outflows in Radio-Quiet Active Galactic Nuclei (2006, background): “It is also a famous ‘‘superwind’’ galaxy, evidenced by optical emission-line gas, figure-eight-shaped radio lobes, and an X-ray-emitting cone, all aligned and extended along the galaxy minor axis (Duric & Seaquist 1988; Cecil et al. 2001, 2002; Irwin& Saikia 2003).”
Outflows in Infrared-Luminous Starbursts at z < 0.5. II. Analysis and Discussion (2005, background): “We suggest that there is a good possibility that there is (or was) material of higher velocities, as is seen in local starburst-driven superwinds like that in NGC 3079 at velocities of up to 1500 km s 1 (Veilleux et al. 1994; Cecil et al. 2001).”
Observations of feedback from radio-quiet quasars - I. Extents and morphologies of ionized gas nebulae (2013, background): “Jets are frequently implicated in strong interactions with galactic interstellar matter (Oosterloo et al. 2000), in exciting the gas through shocks (Cecil et al. 2001) and in producing outflows of gas from the host galaxy, often on scales of several kpc (Baum et al. 1990, 1992; McCarthy 1993;…”
The Large-Scale Bipolar Wind in the Galactic Center (2002, background): “The explicit dependence of derived quantities on filling factors can be found in Cecil et al. (2001, 2002).”
Quasar feedback and the origin of radio emission in radio-quiet quasars (2014, background): “For comparison, the mechanical luminosity necessary to inflate the bubbles in NGC 3079 (Cecil et al. 2001) is ∼ 30 lower than our median Lwind, whereas that inferred for “the Fermi bubbles” in the Milky Way is 105 times lower than our Lwind.”
Unusual Broad Absorption Line Quasars from the Sloan Digital Sky Survey (2002, background): “A combination of disk obscuration and patchy line-emitting gas in the outflow could then explain why only blueshifted line emission is seen (e.g., NGC 3079; Veilleux, Shopbell, & Miller 2001; Cecil et al. 2001).”
A High Spatial Resolution X-Ray and Hα Study of Hot Gas in the Halos of Star-forming Disk Galaxies. I. Spatial and Spectral Properties of the Diffuse X-Ray Emission (2003, background): “…Heckman et al. 1990; Filippenko & Sargent 1992; Veilleux et al. 1994), subsequently dramatically imaged by the Hubble Space Telescope (HST ) WFPC2 (Cecil et al. 2001), and there was suggestive evidence for bright structured diffuse X-ray emission in the same region from ROSAT HRI observations…”
The Vertical Structure of Warm Ionised Gas in the Milky Way (2008, background): “These small cloudlets may correspond to the “drizzle” of ionised gas accreting into the halo proposed by Bland-Hawthorn et al. (2007), or to the extraplanar droplets and clumps of Hα seen in observations of some edge-on spiral galaxies (Ferguson et al. 1996; Cecil et al. 2001).”
The SAMI Galaxy Survey: shocks and outflows in a normal star-forming galaxy (2014, background): “In classical nearby systems such as M82, NGC253, NGC1482, NGC3079 and many others, conical bipolar structures extending up to a few kiloparsecs beyond stellar disks are commonly seen (e.g., Bland & Tully 1988; Westmoquette, Smith & Gallagher 2011; Veilleux & Rupke 2002; Cecil et al. 2001).”
EVIDENCE FOR UBIQUITOUS COLLIMATED GALACTIC-SCALE OUTFLOWS ALONG THE STAR-FORMING SEQUENCE AT z ∼ 0.5 (2013, background): “…detailed shape of these flows with our data, we infer that they take a roughly biconical form, as this morphology is predicted by the simulations mentioned above, and has been observed around numerous local starburst galaxies (e.g., Walter et al. 2002; Veilleux & Rupke 2002; Cecil et al. 2001).”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, background): “…data indicatethat even Seyfert II ULIRGs in which large-scale winds may be driven by star formation have central, AGN-driven outflows (Cecil et al. 2001; Rupke et al. 2005), and observations at optical, X-ray, and radio wavelengths (Colbert et al. 1996a,b, 1998; Whittle & Wilson…”