Extra-planar H I in the starburst galaxy NGC 253

Boomsma, Rense; Oosterloo, Thomas; Fraternali, Filippo; Hulst, van der Thijs; Sancisi, R.

doi:10.1051/0004-6361:20041715

Cited by 77 publications

(95 citation statements)

References 24 publications

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“…The shape of the radio halo in our MWA radio images (Figure 2) resembles the "horn-like" or "X-shaped" structure seen at gigahertz radio frequencies , in H I (Boomsma et al 2005;Lucero et al 2015), X-rays (Fabbiano 1988;Pietsch et al 2000;Bauer et al 2008), Hα (G. Meurer, private communication; Figure 2), UV (Hoopes et al 2005), and far-IR (Kaneda et al 2009). …”

Section: Halo Morphologysupporting

confidence: 59%

Spectral Energy Distribution and Radio Halo of NGC 253 at Low Radio Frequencies

Kapińska

Staveley‐Smith

Crocker

et al. 2017

ApJ

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We present new radio continuum observations of NGC253 from the Murchison Widefield Array at frequencies between 76 and 227 MHz. We model the broadband radio spectral energy distribution for the total flux density of NGC253 between 76 MHz and 11 GHz. The spectrum is best described as a sum of a central starburst and extended emission. The central component, corresponding to the inner 500 pc of the starburst region of the galaxy, is best modeled as an internally free-free absorbed synchrotron plasma, with a turnover frequency around 230 MHz. The extended emission component of the spectrum of NGC253 is best described as a synchrotron emission flattening at low radio frequencies. We find that 34% of the extended emission (outside the central starburst region) at 1 GHz becomes partially absorbed at low radio frequencies. Most of this flattening occurs in the western region of the southeast halo, and may be indicative of synchrotron self-absorption of shock-reaccelerated electrons or an intrinsic low-energy cutoff of the electron distribution. Furthermore, we detect the large-scale synchrotron radio halo of NGC253 in our radio images. At 154-231 MHz the halo displays the well known X-shaped/horn-like structure, and extends out to ∼8 kpc in the z-direction (from the major axis).

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Section: Halo Morphologysupporting

confidence: 59%

Spectral Energy Distribution and Radio Halo of NGC 253 at Low Radio Frequencies

Kapińska

Staveley‐Smith

Crocker

et al. 2017

ApJ

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“…This cycle (i.e., the expulsion and the rain-back of gas) could be responsible for the assembly of an extra-planar gas reservoir. This process could be somewhat analogous to that observed with deep observations of HI 21 cm line emission in several nearby disk galaxies, where neutral hydrogen gas is deposited into the galaxy's halo environment mainly by stellar feedback (in the most extreme cases out to a few tens of kpc above the main galaxy disk; e.g., Fraternali et al 2002Fraternali et al , 2005Boomsma et al 2005;Oosterloo et al 2007;Fraternali & Binney 2008). This extra-planar neutral gas is characterized by slower rotation compared to the galaxy disk (most pronounced at small galactic radii), it can have an asymmetric distribution, and it may contain up to ∼10 9 M of neutral gas (in some cases up to ∼30% of the galaxy's total HI content; see Oosterloo et al 2007;Boomsma et al 2008 for examples).…”

Section: Outflow Mass Rate and The Ism/igm Metal Enrichmentsupporting

confidence: 59%

Spatially resolved kinematics, galactic wind, and quenching of star formation in the luminous infrared galaxy IRAS F11506-3851

Cazzoli

Arribas

Colina

et al. 2014

A&A

105

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We present a multi-wavelength integral field spectroscopic (IFS) study of the low-z luminous infrared galaxy IRAS F11506-3851 (ESO 320-G030) on the basis of the moderate spectral resolution observations (R ∼ 3400−4000) taken with the VIMOS and SINFONI instruments at the ESO VLT. The morphology and the 2D kinematics of the gaseous (neutral and ionized) and stellar components have been mapped in the central regions (<3 kpc) using the NaDλλ5890, 5896 Å absorption doublet, the Hαλ6563 Å line, and the near-IR CO(2-0)λ2.293 µm and CO(3-1)λ2.322 µm bands. The kinematics of the ionized gas and the stars are dominated by rotation, with large observed velocity amplitudes (∆V(Hα) = 203 ± 4 km s −1 ; ∆V(CO) = 188 ± 11 km s −1 , respectively) and centrally peaked velocity dispersion maps (σ c (Hα) = 95 ± 4 km s −1 and σ c (CO) = 136 ± 20 km s −1 ). The stars lag behind the warm gas and represent a dynamically hotter system, as indicated by the observed V/σ ratios (4.5 and 2.4 for the gas and the stars, respectively). Thanks to these IFS data we have disentangled the contribution of the stars and the interstellar medium to the NaD feature, finding that it is dominated by absorption of neutral gas clouds in the interstellar medium (∼2/3 of total EW). The 2D kinematics of the neutral gas shows a complex structure dominated by two main components. On the one hand, the thick slowly rotating disk (∆V(NaD) = 81 ± 12 km s −1 ) lags significantly compared to the ionized gas and the stars, and it has an irregular and off-center velocity dispersion map (with values of up to ∼150 km s −1 at ∼1 kpc from the nucleus). On the other hand, a kpc-scale neutral gas outflow perpendicular to the disk, as is revealed by the large blueshifted velocities (in the range 30−154 km s −1 ) observed along the galaxy's semi-minor axis (within the inner 1.4 kpc). On the basis of a simple free wind scenario, we derive an outflowing mass rate (Ṁ w ) in neutral gas of about 48 M yr −1 . Although this implies a global mass loading factor (i.e., η =Ṁ w /SFR) of ∼1.4, the 2D distribution of the ongoing SF as traced by the Hα emission map suggests a much larger value of η associated with the inner regions (R < 200 pc), where the current observed star formation (SF) represents only ∼3 percent of the total. However, the relatively strong emission by supernovae in the central regions, as traced by the [FeII] emission, indicates recent strong episodes of SF. Therefore, our data show clear evidence of the presence of a strong outflow with large loading factors associated with the nuclear regions, where recent starburst activity took place about 7 Myr ago, although it currently shows relatively modest SF levels. All together these results strongly suggest that we are witnessing (nuclear) quenching due to SF feedback in IRAS F11506-3851. However, the relatively large mass of molecular gas detected in the nuclear region via the H 2 1−0S(1) line suggests that further episodes of SF may take place again.

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“…Superwind cones are commonly observed in X-rays, radio continuum and Hα but infrequently in HI. In the case of NGC 253, HI has been observed to be confined within the optical disk and to outline the superwind cone of ionized gas in one half of the galaxy (Boomsma et al 2004). Another study has shown that significant amounts of HI is observed to be in the halos of spiral galaxies with active star formation (Fraternali et al 2001).…”

Section: Starburst Driven Superwindmentioning

confidence: 99%

GMRT observations of the group Holmberg 124: Evolution by tidal forces and ram pressure?

Kantharia

Ananthakrishnan

Nityananda

et al. 2005

A&A

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Abstract. We report new radio continuum and 21 cm HI observations using the Giant Metrewave Radio Telescope (GMRT) of the group Holmberg 124 (Ho 124) comprising four late-type galaxies, namely NGC 2820, Mrk 108, NGC 2814 and NGC 2805. The three galaxies, NGC 2820, Mrk 108 and NGC 2814 which are closely located in the sky plane have clearly undergone tidal interactions as seen from the various morphological tidal signatures and debris. Moreover we note various features in the group members which we believe might be due to ram pressure. In this paper, we describe four interesting results emerging from our observations: a) detection of the tidal radio continuum bridge at 330 MHz connecting the galaxies NGC 2820+Mrk 108 with NGC 2814. The radio bridge was discovered at 1465 MHz by van der Hulst & Hummel (1985, A&A, 150, 17). We find that the bridge has a fairly steep spectrum with a spectral index α (S ∝ ν α ) of −1.8 +0.3 −0.2 which is much steeper than the −0.8 quoted by van der Hulst & Hummel (1985); b) detection of other tidal features like the tilted HI and radio continuum disk of NGC 2814, a HI streamer and a radio continuum tail arising from the south of NGC 2814. We also report the detection of a possible tidal dwarf galaxy in HI; c) sharp truncation in the HI distribution in the south of NGC 2820 and in the HI and radio continuum distribution in the north of NGC 2814. The optical disks in both the cases look undisturbed. As pointed out by Davis et al. (1997, AJ, 114, 613), ram pressure affects different components of the interstellar medium to varying degrees. Simple estimates of pressure in different components of the interstellar medium (radio continuum, Hα and HI) in NGC 2820 indicate that ram pressure will significantly influence HI; d) detection of a large one-sided HI loop to the north of NGC 2820. No radio continuum emission or Hα emission is associated with the HI loop. We discuss various scenarios for the origin of this loop including a central starburst, ram pressure stripping and tidal interaction. We do not support the central starburst scenario since the loop is not detected in ionized gas. Using the upper limit on X-ray luminosity of Ho 124 (Mulchaey et al. 2003, ApJS, 145, 39), we estimate an upper limit on the intragroup medium (IGrM) density of 8.8 × 10 −4 cm −3 . For half this electron density, we estimate the ram pressure force of the IGrM to be comparable to the gravitational pull of the disk of NGC 2820. Since tidal interaction has obviously influenced the group, we suggest that the loop could have formed by ram pressure stripping if tidal effects had reduced the surface density of HI in NGC 2820. From the complex observational picture of Ho 124 and the numerical estimates, we suggest that the evolution of the Ho 124 group may be governed by both tidal forces due to the interaction and the ram pressure due to motion of the member galaxies in the IGrM and that the IGrM densities should not be too low (i.e. ≥4 × 10 −4 ). However this needs to be verified by further observations.

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Extra-planar H I in the starburst galaxy NGC 253

Cited by 77 publications

References 24 publications

Spectral Energy Distribution and Radio Halo of NGC 253 at Low Radio Frequencies

Spectral Energy Distribution and Radio Halo of NGC 253 at Low Radio Frequencies

Spatially resolved kinematics, galactic wind, and quenching of star formation in the luminous infrared galaxy IRAS F11506-3851

GMRT observations of the group Holmberg 124: Evolution by tidal forces and ram pressure?

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