Exploring the dust content of galactic haloes with <i>Herschel</i> – IV. NGC 3079

Veilleux, Sylvain; Meléndez, M.; Stone, Myra; Cecil, Gerald; Hodges-Kluck, Edmund; Bland-Hawthorn, Joss; Bregman, Joel N.; Heitsch, Fabian; Martin, Crystal L.; Mueller, Thomas; Rupke, David S. N.; Sturm, E.; Tanner, Ryan; Engelbracht, C. W.

doi:10.1093/mnras/stab2881

Cited by 5 publications

(5 citation statements)

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“…The boundary of such a bubble may be related to the Xshaped structures centred on the nucleus, but with footpoints at a galactocentric radius r 0 . Thus then would define the midplane flow radius, which may be the boundary of this outflow (Veilleux et al 2021, see also Fig. 21).…”

Section: Motivationmentioning

confidence: 99%

The radio continuum perspective on cosmic-ray transport in external galaxies

Heesen

2021

Astrophys Space Sci

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Radio continuum observations of external galaxies provide us with an excellent outside view on the distribution of cosmic-ray electrons in the disc and halo. In this review, we summarise the current state of what we have learned from modelling such observations with cosmic-ray transport, paying particular attention to the question to what extent we can exploit radio haloes when studying galactic winds. We have developed the user-friendly framework spinnaker to model radio haloes with either pure advection or diffusion, allowing us to study both diffusion coefficients and advection speeds in nearby galaxies. Using these models, we show that we can identify galaxies with winds using both morphology and radio spectral indices of radio haloes. Advective radio haloes are ubiquitous, indicating that already fairly low values of the star formation rate (SFR) surface density ($\Sigma_{ \mathrm{SFR}}$ Σ SFR ) can trigger galactic winds. The advection speeds scale with SFR, $\Sigma_{\mathrm{SFR}}$ Σ SFR , and rotation speed as expected for stellar feedback-driven winds. Accelerating winds are in agreement with our radio spectral index data, but this is sensitive to the magnetic field parametrisation, so that constant wind speeds cannot be ruled out either. The question to what extent cosmic rays can be a driving force behind winds is still an open issue and we discuss only in passing how a simple iso-thermal wind model could fit our data. Nevertheless, the comparison with inferences from observations and theory looks promising with radio continuum offering a complementary view on galactic winds. We finish with a perspective on future observations and challenges lying ahead.

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Section: Motivationmentioning

confidence: 99%

The radio continuum perspective on cosmic-ray transport in external galaxies

Heesen

2021

Astrophys Space Sci

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“…We therefore need to investigate the energetics associated with the starburst of NGC 1808 and the outflow. We adopt the isothermal sheet model used by Meléndez et al (2015) and Veilleux et al (2021) to calculate the potential energy required to lift a mass out of the galactic plane,…”

Section: Discussion: Origin Of the Extraplanar Dusty Filamentsmentioning

confidence: 99%

“…The mass-loading factor we find for the dusty outflow in NGC 1808 is therefore typical of starburst galaxies, given the rather large uncertainties on this estimate. For comparison with an AGN-driven outflow, Veilleux et al (2021) find a mass-loading factor in NGC 3079 above 100. The discrepancy between this value and what we find in NGC 1808 is in line with the conclusions of prior work that the AGN in NGC 1808 is rather weak (Salak et al 2018) and energetically not important in driving the observed largescale outflow.…”

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confidence: 94%

“…The Herschel Science Archive (HSA) 3 of the Herschel Space Observatory (Herschel; Pilbratt et al 2010) has proven to be of great value for studying the distribution and properties of the cool dust with temperatures T ∼ 10-100 K in and around nearby galaxies. In particular, deep Herschel observations of edge-on disk galaxies have revealed extraplanar dust typically extending up to heights |z| ∼ 3 kpc, but sometimes up to 10-25 kpc (Roussel et al 2010;Meléndez et al 2015;McCormick et al 2018;Veilleux et al 2021;Yoon et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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Giant Biconical Dust Filaments in the Starburst Galaxy NGC 1808

Kane,

Veilleux

2024

ApJ

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We present the results from an analysis of multiwavelength archival data on the multiphase outflow in the starburst galaxy NGC 1808. We report the detection at 70 and 100 μm of dust filaments that extend up to ∼13 kpc from the galactic midplane and trace an edge-brightened biconical structure along the minor axis of the galaxy. The inner filaments are roughly cospatial with previously identified optical dust filaments, extraplanar polycyclic aromatic hydrocarbon emission, and neutral and ionized gaseous outflows. The 70/160 μm flux ratio, a proxy for the dust temperature, is elevated along the edges of the cones, indicating that the dusty medium has been driven out of the central regions of these cones and is possibly shock-heated by a large-scale outflow. We establish lower limits on the extraplanar dust mass and mean height above the stellar disk of log ( M d / M ⊙ ) = 6.48 and ∣ z ∣ ∼ 5 kpc. The energy requirement of (5.1–9.6) × 1056 erg needed to lift the dusty material, assuming a Milky Way–like dust-to-gas ratio, can be supplied by the current starburst, with a measured star formation rate of 3.5–5.4 M ⊙ yr−1 over a timescale of (4–26) ξ −1 Myr, where ξ is the efficiency of energy transfer. We conclude that a starburst-driven outflow is the most likely mechanism by which the dust features were formed.

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“…Es-timates of the extraplanar ( > ∼ 1 kpc) FIR emission in edge-on galaxies give similar numbers. For instance, the sum of the FIR fluxes from extraplanar regions around the X-shaped structure in the galaxy NGC 3079 with its SFR≈ 2.6 ⊙ yr −1 (Veilleux et al 2021), results in ∼ 2 × 10 7 SFR in solar units. A similar value ∼ 4 × 10 7 SFR can be inferred from the data for the halo of the galaxy NGC 891 presented by Yoon et al (2021, see their Table 3).…”

Section: 21)mentioning

confidence: 99%

Disc-halo gas outflows driven by stellar clusters as seen in multiwavelength tracers

Vasiliev¹,

Drozdov²,

Nath³

et al. 2023

Preprint

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We consider the dynamics of and emission from growing superbubbles in a stratified interstellar gaseous disc driven by energy release from supernovae explosions in stellar clusters with masses = 10 5 − 1.6 × 10 6 ⊙ . Supernovae are spread randomly within a sphere of = 60 pc, and inject energy episodically with a specific rate 1/130 −1 ⊙ proportional to the star formation rate (SFR) in the cluster. Models are run for several values of SFR in the range 0.01 to 0.1 ⊙ yr −1 , with the corresponding average surface energy input rate ∼ 0.04 − 0.4 erg cm −2 s −1 . We find that the discrete energy injection by isolated SNe are more efficient in blowing superbubbles: asymptotically they reach heights of up to 3 to 16 kpc for = 10 5 − 1.6 × 10 5 ⊙ , correspondingly, and stay filled with a hot and dilute plasma for at least 30 Myr. During this time they emit X-ray, H and dust infrared emission. X-ray liminosities ∝ SFR 3/5 that we derive here are consistent with observations in star-forming galaxies. Even though dust particles of small sizes ≤ 0.03 m are sputtered in the interior of bubbles, larger grains still contribute considerably ensuring the bubble luminosity IR /SFR ∼ 5 × 10 7 ⊙ −1 ⊙ yr. It is shown that the origin of the North Polar Spur in the Milky Way can be connected with activity of a cluster with the stellar mass of ∼ 10 5 ⊙ and the SFR ∼ 0.1 ⊙ yr −1 some 25-30 Myr ago. Extended luminous haloes observed in edge-on galaxies (NGC 891 as an example) can be maintained by disc spread stellar clusters of smaller masses * < ∼ 10 5 ⊙ .

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Exploring the dust content of galactic haloes with Herschel – IV. NGC 3079

Cited by 5 publications

References 91 publications

The radio continuum perspective on cosmic-ray transport in external galaxies

The radio continuum perspective on cosmic-ray transport in external galaxies

Giant Biconical Dust Filaments in the Starburst Galaxy NGC 1808

Disc-halo gas outflows driven by stellar clusters as seen in multiwavelength tracers

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