A Spiral-Like Disk of Ionized Gas in IC 1459: Signature of a Merging Collision?

Goudfrooij, Paul; Nørgaard-Nielsen, H. U.; Jørgensen, H. E.; Hansen, L.; Jong, T. de

doi:10.1017/s0252921100005121

Cited by 30 publications

(55 citation statements)

References 14 publications

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“…In addition to the dust located at its center, IC1459 has large strip of dust lining from the south-east to the north-west on its west side. Goudfrooij et al (1990) identified some potential spiral arms in Hα maps of IC1459 that extend about 40" away from its center. The location of the two largest Hα arms seems to coincide with the location of the structures present north of the galaxy center in the 160µm map, although the FIR structures do not resemble closely the shape of spiral arms.…”

Section: Ic1459 Analysismentioning

confidence: 99%

SPECTRAL ENERGY DISTRIBUTION MAPPING OF TWO ELLIPTICAL GALAXIES ON SUB-kpc SCALES

Amblard¹,

Temi²,

Gaspari³

et al. 2016

ApJ

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We use high-resolution Herschel-PACS data of 2 nearby elliptical galaxies, IC1459 & NGC2768 to characterize their dust and stellar content. IC1459 & NGC2768 have an unusually large amount of dust for elliptical galaxies (1 to 3×10 5 M ), this dust is also not distributed along the stellar content. Using data from GALEX (ultra-violet) to PACS (far-infrared), we analyze the spectral energy distribution (SED) of these galaxies with CIGALEMC as a function of the projected position, binning images in 7.2" pixels. From this analysis, we derive maps of SED parameters, such as the metallicity, the stellar mass, the fraction of young star and the dust mass. The larger amount of dust in FIR maps seems related in our model to a larger fraction of young stars which can reach up to 4% in the dustier area. The young stellar population is fitted as a recent (∼ 0.5 Gyr) short burst of star formation for both galaxies. The metallicities, which are fairly large at the center of both galaxies, decrease with the radial distance with fairly steep gradient for elliptical galaxies.

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Section: Ic1459 Analysismentioning

confidence: 99%

SPECTRAL ENERGY DISTRIBUTION MAPPING OF TWO ELLIPTICAL GALAXIES ON SUB-kpc SCALES

Amblard¹,

Temi²,

Gaspari³

et al. 2016

ApJ

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“…The diffuse X-ray emission has an ellipticity of about e $ 0:15, and the position angle twists from P:A: $ 135 for r < 50 00 to P:A: $ 110 at larger radii (Buote et al 2002). The stellar light has e ¼ 0:45 AE 0:05 and P:A: ¼ 142 AE 3 , and the distribution of globular clusters follows e ¼ 0:5 AE 0:1 and P:A: ¼ 147 AE 10 ( Kissler-Patig, Richtler, & Hilker 1996;Peletier et al 1990;Goudfrooij 1994). Figure 6a shows the angular distribution of X-ray sources.…”

Section: Spatial Distributionmentioning

confidence: 99%

X‐Ray Source Population in the Elliptical Galaxy NGC 720 withChandra

Jeltema

Canizares

Buote

et al. 2003

ApJ

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With a Chandra ACIS-S3 observation, we detect 42 X-ray point sources in the elliptical galaxy NGC 720, including a possible central source. Most of these sources will be low-mass X-ray binaries, and 12 are located within 2 00 of globular cluster candidates. We investigate both the hardness ratios and combined spectra of the sources. They exhibit a distribution of X-ray colors similar to those seen in other early-type galaxies. We find that there is a population of highly absorbed sources located at large distances from the center of the galaxy. The overall spatial distribution of sources is consistent with the ellipticity and position angle of the galaxy, but the sources appear to form several arcs. NGC 720 contains nine ultraluminous sources (ULXs; L X ! 10 39 ergs s À1 ). This number is more than have previously been detected in an early-type galaxy but similar to the number seen in the Antennae merger system. The ratio L ULX =L B for NGC 720 is more than double the ratio for the S0 galaxy NGC 1553 and a factor of 7 higher than for the elliptical galaxy NGC 4697, although uncertainties in the distance and the source spectral properties could bring these ratios into agreement. The X-ray source luminosity function is also nearly as flat as those seen in disk and merger systems. The large number of ULXs in NGC 720 and its relatively flat X-ray luminosity function may provide evidence against the association of all ULXs with young stars. We also see a possible high-luminosity break in the luminosity function at 2 Â 10 39 h À2 50 ergs s À1 .

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“…The IC 1459 galaxy itself has a number of peculiar features, hinting at disturbances due to interactions and/or merging: twisted isophotes first noticed by Williams & Schwarzschild (1979) and Franx et al (1989), a fast counter-rotating stellar core (Franx & Illingworth 1988), faint stellar shells (Malin 1985) and a large H + N [iii] emission-line disc showing a weak spiral structure (Goudfrooij et al 1990). Furthermore, IC 1459 hosts a bright radio source, PKS 2254-367, characterised by two symmetric radio jets, whose activity may have been triggered by the same events that gave the galaxy its peculiar morphology and kinematics.…”

Section: The Ic 1459 Galaxy Groupmentioning

confidence: 99%

H i debris in the IC 1459 galaxy group

Saponara

Koribalski

Benaglia

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present H i synthesis imaging of the giant elliptical galaxy IC 1459 and its surroundings with the Australia Telescope Compact Array (ATCA). Our search for extended H i emission revealed a large complex of H i clouds near IC 1459, likely the debris from tidal interactions with neighbouring galaxies. The total H i mass (∼ 10 9 M ) in the detected clouds spans 250 kpc from the north-east of the gas-rich spiral NGC 7418A to the south-east of IC 1459. The extent and mass of the H i debris, which shows rather irregular morphology and kinematics, are similar to those in other nearby groups. Together with H i clouds recently detected near two other IC 1459 group members, namely IC 5270 and NGC 7418, using Phased-Array Feeds (PAFs) on the Australian Square Kilometer Array Pathfinder (ASKAP), the detected debris make up a significant fraction of the group's intergalactic medium.

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A Spiral-Like Disk of Ionized Gas in IC 1459: Signature of a Merging Collision?

Cited by 30 publications

References 14 publications

SPECTRAL ENERGY DISTRIBUTION MAPPING OF TWO ELLIPTICAL GALAXIES ON SUB-kpc SCALES

SPECTRAL ENERGY DISTRIBUTION MAPPING OF TWO ELLIPTICAL GALAXIES ON SUB-kpc SCALES

X‐Ray Source Population in the Elliptical Galaxy NGC 720 withChandra

H i debris in the IC 1459 galaxy group

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