Deep Near‐Infrared Imaging and Photometry of the Antennae Galaxies with WIRC

Brandl, Bernhard R.; Clark, David M.; Eikenberry, S. S.; Wilson, John C.; Henderson, C.; Barry, D. J.; Houck, J. R.; Carson, J.; Hayward, T. L.

doi:10.1086/497357

Cited by 28 publications

(36 citation statements)

References 19 publications

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“…This basically agrees with star cluster age distributions given by Kassin et al (2003), Brandl et al (2005), and Mengel et al (2005). The locations of these sites of star formation all do not coincide with the CO clouds.…”

Section: Near-infraredsupporting

confidence: 85%

The interstellar medium of the Antennae galaxies

Schulz

Henkel

Muders

et al. 2007

A&A

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To study the properties of the interstellar medium in the prototypical merging system of the Antennae galaxies (NGC 4038 and NGC 4039), we have obtained 12 CO (1-0), (2-1) and (3-2) line maps, as well as a map of the 870µm continuum emission. Our results are analysed in conjunction with data from X-ray to radio wavelengths. In order to distinguish between exact coincidence and merely close correspondence of emission features, we compare the morphological structure of the different emission components at the highest available angular resolution. To constrain the physical state of the molecular gas, we apply models of photon dominated regions (PDRs) that allow us to fit CO and [Cii] data, as well as other indicators of widespread PDRs in the Antennae system, particularly within the super giant molecular cloud (SGMC) complexes of the interaction region (IAR) between the two galaxies. The modeled clouds have cores with moderately high gas densities up to 4 10 4 cm −3 and rather low kinetic temperatures (≤25K). At present, all these clouds, including those near the galactic nuclei, show no signs of intense starburst activity. Thermal radio or mid-infrared emission are all observed to peak slightly offset from the molecular peaks. The total molecular gas mass of the Antennae system adds up to ∼10 10 M ⊙ . In the vicinity of each galactic nucleus, the molecular gas mass, 1 -2 10 9 M ⊙ , exceeds that of the Galactic centre region by a factor of almost 100. Furthermore, the gas does not seem to deviate much from the N H 2 /I CO ratio typical of the disk of our Galaxy rather than our Galactic centre. Alternative heating mechanisms with respect to PDR heating are discussed.

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Section: Near-infraredsupporting

confidence: 85%

The interstellar medium of the Antennae galaxies

Schulz

Henkel

Muders

et al. 2007

A&A

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“…We found that this knot has infrared colors even warmer than that of the YSCC in ARP 24, based on archival Spitzer data (PI: G. Fazio; see also Wang et al 2004). Its very red near-infrared color (J − Ks = 1.86) indicates that it suffers from heavy dust extinction (Brandl et al 2005). Thus, we speculate that some star clusters in galaxies which are very young and optically faint caused by heavy dust extinctions may also have warm infrared colors like the YSCC we found in ARP 24.…”

Section: Pah and Warm Dust Emissionmentioning

confidence: 49%

Multiwavelength Study of Young Massive Star Clusters in the Interacting Galaxy Arp 24

Cao

2007

Astron J

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We made a multi-wavelength study of young massive star clusters (YSCs) in the interacting galaxy ARP 24, using the optical and ultraviolet images from Hubble Space Telescope (HST), Sloan Digital Sky Survey, and Galaxy Evolution Explorer; the mid-infrared images from Spitzer Space Telescope; and the narrowband Hα image and optical spectra from the NAOC 2.16 m telescope. Based on the HST images, we found that the brightest infrared knot in ARP 24 is associated with a complex of five young massive star clusters, within a region of ∼ 0.95 ′′ radius (127pc) in size. The ages and masses of the star clusters in this complex and other regions were estimated using HST broadband photometries and the Starburst99 synthesis models. The star clusters in this complex are very young (within ages of ∼ 3-5 Myr) and massive (masses of ∼10 5 M ⊙ ). The ionization parameter and metallicity of the complex were estimated using the emission line ratios, and the star formation rates were calculated using monochromatic 24µm, FUV, and Hα line luminosities. We speculate that ARP 24 may formed by a retrograde fly-by encounter indicated by its one-armed appearance and fanlike structure, and the formation of the YSCs in this galaxy is triggered by the interaction. The clusters in the YSC complex may formed in a single giant molecular cloud simultaneously. From the ultraviolet to mid-infrared spectral energy distributions, we found that the region of the YSC complex is relatively bluer in optical and has higher 24µm dust emission relative to the starlight and 8µm emission. This warm infrared color may due to strong UV radiation field or other mechanisms (e.g., shocks) within this region which may destroy the Polycyclic Aromatic Hydrocarbons and enhance the small grain emission at 24µm.

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“…This system is one of the most spectacular examples of gas-rich major mergers as well as being the closest (distance=22±3 Mpc, Schweizer et al 2008). The system has a total infrared luminosity of log(L ir /L ) = 10.86 (Sanders et al 2003) approaching that of a luminous infrared galaxy, and is subject of heavy and variable attenuation (Brandl et al 2005). It therefore presents a good target for the search of extragalactic DIBs.…”

Section: Introductionmentioning

confidence: 99%

Diffuse interstellar bands λ5780 and λ5797 in the Antennae Galaxy as seen by MUSE

Monreal-Ibero

Weilbacher

Wendt

2018

A&A

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Context. Diffuse interstellar bands (DIBs) are faint spectral absorption features of unknown origin. Research on DIBs beyond the Local Group is very limited and will surely blossom in the era of the Extremely Large Telescopes. However, we can already start paving the way. One possibility that needs to be explored is the use of high-sensitivity integral field spectrographs. Aims. Our goals are twofold. First, we aim to derive reliable mapping of at least one DIB in a galaxy outside the Local Group. Second, we want to explore the relation between DIBs and other properties of the interstellar medium (ISM) in the galaxy. Methods. We use Multi Unit Spectroscopic Explorer (MUSE) data for the Antennae Galaxy, the closest major galaxy merger. High signal-to-noise spectra were created by co-adding the signal of many spatial elements with the Voronoi binning technique. The emission of the underlying stellar population was modelled and substracted with the STARLIGHT spectral synthesis code. Flux and equivalent width of the features of interest were measured by means of fitting to Gaussian functions. Results. To our knowledge, we have derived the first maps for the DIBs at λ5780 and λ5797 in galaxies outside the Local Group. The strongest of the two DIBs (at λ5780) was detected in an area of ∼ 0.6 , corresponding to a linear scale of ∼ 25 kpc 2 . This region was sampled using >200 out of ∼1200 independent lines of sight. The DIB λ5797 was detected in >100 independent lines of sight. Both DIBs are associated with a region of high emission in the H i 21 cm line, implying a connection between atomic gas and DIBs, as the correlations in the Milky Way also suggest. Conversely, there is mild spatial association between the two DIBs and the molecular gas, in agreement with results for our Galaxy that indicate a lack of correlation between DIBs and molecular gas. The overall structures for the DIB strength distribution and extinction are comparable. Within the system, the λ5780 DIB clearly correlates with the extinction, and both DIBs follow the relationship between equivalent width and reddening when data for several galaxies are considered. This relationship is tighter when comparing only with galaxies with metallicities close to solar. Unidentified infrared emission bands (UIBs, likely caused by polycyclic aromatic hydrocarbons (PAHs)) and the λ5780 and λ5797 DIBs show similar but not identical spatial distributions. We attribute the differences to extinction effects without necessarily implying a radically different nature of the respective carriers. Conclusions. The results illustrate the enormous potential of integral field spectrographs for extragalactic DIB research.

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Deep Near‐Infrared Imaging and Photometry of the Antennae Galaxies with WIRC

Cited by 28 publications

References 19 publications

The interstellar medium of the Antennae galaxies

The interstellar medium of the Antennae galaxies

Multiwavelength Study of Young Massive Star Clusters in the Interacting Galaxy Arp 24

Diffuse interstellar bands λ5780 and λ5797 in the Antennae Galaxy as seen by MUSE

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