X-Ray Emission From the Taffy (Vv254) Galaxies and Bridge

Appleton, P. N.; Lanz, Lauranne; Bitsakis, T.; Wang, Junfeng; Peterson, Bradley W.; Lisenfeld, U.; Alatalo, Katherine; Guillard, P.; Boulanger, F.; Cluver, Michelle; Gao, Yu; Hélou, G.; Ogle, Patrick; Struck, Curtis

doi:10.1088/0004-637x/812/2/118

Cited by 14 publications

(36 citation statements)

References 89 publications

(194 reference statements)

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“…These values are in good agreement with those of Appleton et al (2015) who estimated the SFR using several different methods.…”

Section: Star Formation In the Taffy Systemsupporting

confidence: 89%

“…It is possible that this emission is bridge material superimposed on the northern disk, as it shares similar properties to other material in the bridge. X-ray emission, which we suggested was shock-heated gas left over from the initial collision between the Taffy galaxies (Appleton et al 2015), also occupies this region of the northwest disk of UGC 12915 and the bridge. To compare the PACS spectra of the extracted regions with the Condon et al (1993) and CO data from BIMA CO(1-0) (Gao et al 2003), we obtained calibrated data cubes of both sets of observations and performed extractions over similar areas to those of Figure 1.…”

mentioning

confidence: 77%

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Herschel Spectroscopy of the Taffy Galaxies (UGC 12914/12915 = VV 254): Enhanced [C ii] Emission in the Collisionally Formed Bridge

Peterson¹,

Appleton

Bitsakis

et al. 2018

ApJ

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neutral carbon lines, and weakly detects high-J CO transitions in the bridge. These results indicate that the bridge is composed of a warm multi-phase medium consistent with shock and turbulent heating. Despite low star formation rates in the bridge, the [C II] emission appears to be enhanced, reaching [C II]/FIR ratios of 3.3% in parts of the bridge. Both the [C II] and [O I] lines show broad intrinsic multi-component profiles, similar to those seen in previous CO (1-0) and H I observations. The [C II] emission shares similar line profiles with both the double-peaked H I profiles and shares a high-velocity component with single-peaked CO profiles in the bridge, suggesting that the [C II] emission originates in both the neutral and molecular phases. We show that it is feasible that a combination of turbulently heated H 2 and high column-density H I, resulting from the galaxy collision, is responsible for the enhanced [C II] emission.

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“…These values are in good agreement with those of Appleton et al (2015) who estimated the SFR using several different methods.…”

Section: Star Formation In the Taffy Systemsupporting

confidence: 89%

mentioning

confidence: 77%

Herschel Spectroscopy of the Taffy Galaxies (UGC 12914/12915 = VV 254): Enhanced [C ii] Emission in the Collisionally Formed Bridge

Peterson¹,

Appleton

Bitsakis

et al. 2018

ApJ

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“…Numerical models of such a head-on collision between two gas rich galaxies (e.g., Struck 1997) and a detailed model of the Taffy system (Vollmer et al 2012) provide strong support for the idea that the gas left behind in the center of mass frame of the collision would be highly turbulent, and that some would be strongly shock heated. Appleton et al (2015) detected faint extended soft X-ray emission, and several compact point X-ray sources in the bridge, the former being consistent with shock-heated gas that has not had time to completely cool since the collision occurred. Finally, Lisenfeld & Völk (2010) concluded that the radio emission in the bridge could be explained in terms of cosmic rays accelerated in magnetic fields compressed in shocks.…”

Section: Introductionmentioning

confidence: 68%

Evidence for Shock-heated Gas in the Taffy Galaxies and Bridge from Optical Emission-line IFU Spectroscopy

Joshi

Appleton

Blanc

et al. 2019

ApJ

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We present optical IFU observations of the Taffy system (UGC 12914/15); named for the radio emission that stretches between the two galaxies. Given that these gas rich galaxies are believed to have recently collided head-on, the pair exhibits a surprisingly normal total (sub-LIRG) IR luminosity (L FIR ∼ 4.5 × 10 10 L ). Previous observations have demonstrated that a large quantity of molecular and neutral gas have been drawn out of the galaxies into a massive multi-phase bridge. We present, for the first time, spatially resolved spectroscopy of the ionized gas in the system. The results show that the ionized gas is highly disturbed kinematically, with gas spread in two main filaments between the two galaxies. The line profiles exhibit widespread double components in both the bridge and parts of the disks of the galaxies. We investigate the spatial distribution of the excitation properties of the ionized gas using emission-line diagnostic diagrams, and conclude that large quantities (up to 40%) of the emission from the entire system is consistent with gas heated in ∼200 km s −1 shocks. While the shocked gas is mainly associated with the bridge, there is a significant amount of shocked gas associated with both galaxies. Confirming other multi-wavelength indicators, the results suggest that the effects of shocks and turbulence can continue to be felt in a high-speed galaxy collision long after the collision has occurred. The persistence of shocks in the Taffy system may explain the relatively low current star formation rates in the system as a whole.

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“…Soft X-ray emission was observed over the entire bridge with the Chandra telescope as described in Appleton et al (2015). Several individual X-ray sources were also detected, indicative of recent star formation.…”

mentioning

confidence: 92%

Models of multicomponent splash bridges in face-on galaxy disc collisions

Yeager

Struck

2019

Monthly Notices of the Royal Astronomical Society

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We use an inelastic particle code with shocks and cooling calculated on a subgrid level to study the gas in direct collisions between galaxy discs. The interstellar media (ISM) of the discs are modeled with continuous thermal phases. The models produce many unique structures, collectively called splash bridges. They range from central bridge discs to swirled sheets, which resemble those observed in interacting galaxies. These morphologies are sensitive to the rotation, relative mass, disc offsets and the gas structure in the discs. In the case of the Taffy galaxies -NGC 12914/15, extensive observations have revealed radio continuum emitting gas, HI gas, hot X-rays from hot diffuse gas and more H 2 than exists in the Milky Way coexisting in the bridge. The origins of the H 2 and large asymmetric distribution of ISM are not clear. We show that for small disc impact parameters, multiple phases of ISM with densities over many orders of magnitude can be removed from their host galaxies into a Taffy-like bridge. The orientation of the discs initial overlap can have a great effect on the distributions of each phase of ISM. In some cases, the models also predict the creation of a possible 'dark galaxy,' a large flat region of dense ISM far from the stellar disc potential of either galaxy.

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X-Ray Emission From the Taffy (Vv254) Galaxies and Bridge

Cited by 14 publications

References 89 publications

Herschel Spectroscopy of the Taffy Galaxies (UGC 12914/12915 = VV 254): Enhanced [C ii] Emission in the Collisionally Formed Bridge

Herschel Spectroscopy of the Taffy Galaxies (UGC 12914/12915 = VV 254): Enhanced [C ii] Emission in the Collisionally Formed Bridge

Evidence for Shock-heated Gas in the Taffy Galaxies and Bridge from Optical Emission-line IFU Spectroscopy

Models of multicomponent splash bridges in face-on galaxy disc collisions

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