Kinematics of Haro 11: The miniature Antennae

Östlin, Göran; Marquart, Thomas; Cumming, Robert; Fathi, Kambiz; Bergvall, Nils; Adamo, Angela; Amram, P.; Hayes, Matthew

doi:10.1051/0004-6361/201323233

Cited by 35 publications

(13 citation statements)

References 67 publications

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“…Knot C is visually the brightest knot and shows strong Lyα emission (Kunth et al 2003;Östlin et al 2009;Hayes 2015). It appears to be the nucleus of one of the two galaxies in this merging system (James et al 2013;Östlin et al 2015), and Prestwich et al (2015) also identify Knot C as the host of a ULX source with an X-ray luminosity of L X ∼ 5 × 10 40 erg s −1 , dubbed Haro 11 X-2. They suggest that this source may provide enough mechanical power to clear channels through the ISM promoting a low Lyα optical depth.…”

Section: A B or C? Implications For Lyc Escapementioning

confidence: 99%

Haro 11: Where is the Lyman Continuum Source?

Keenan

Oey

Jaskot

et al. 2017

ApJ

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Identifying the mechanism by which high energy Lyman continuum (LyC) photons escaped from early galaxies is one of the most pressing questions in cosmic evolution. Haro 11 is the best known local LyC leaking galaxy, providing an important opportunity to test our understanding of LyC escape. The observed LyC emission in this galaxy presumably originates from one of the three bright, photoionizing knots known as A, B, and C. It is known that Knot C has strong Lyα emission, and Knot B hosts an unusually bright ultraluminous X-ray source, which may be a low-luminosity AGN. To clarify the LyC source, we carry out ionization-parameter mapping (IPM) by obtaining narrow-band imaging from the Hubble Space Telescope WFC3 and ACS cameras to construct spatially resolved ratio maps of [Oiii]/[Oii] emission from the galaxy. IPM traces the ionization structure of the interstellar medium and allows us to identify optically thin regions. To optimize the continuum subtraction, we introduce a new method for determining the best continuum scale factor derived from the mode of the continuumsubtracted, image flux distribution. We find no conclusive evidence of LyC escape from Knots B or C, but instead, we identify a high-ionization region extending over at least 1 kpc from Knot A. Knot A shows evidence of an extremely young age ( 1 Myr), perhaps containing very massive stars (> 100 M ). It is weak in Lyα, so if it is confirmed as the LyC source, our results imply that LyC emission may be independent of Lyα emission.

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Section: A B or C? Implications For Lyc Escapementioning

confidence: 99%

Haro 11: Where is the Lyman Continuum Source?

Keenan

Oey

Jaskot

et al. 2017

ApJ

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“…Another possibility for the Lyα to be intrinsically weak is if the channels through which LyC photons escape are "clean" without any neutral H I gas, making nebu- lar emission like Lyα no longer pumped (Vanzella et al 2012). For example, this scenario could be the case of Haro 11 (z∼0.021, M * ∼ 2.4 × 10 10 M ; Bergvall et al 2006;Östlin et al 2015) which Keenan et al (2017) studied using spatially resolved maps of the emission line ratio [O III]λ5007/[O II]λ3727, finding evidence that the LyC emission may be independent of that of the Lyα. It is unclear, however, the extent to which Haro 11 might be representative of Ion1.…”

Section: Spectrummentioning

confidence: 99%

HST Imaging of the Ionizing Radiation from a Star-forming Galaxy at z = 3.794

Giavalisco

Vanzella³

et al. 2020

ApJ

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We report on the HST detection of the Lyman-continuum (LyC) radiation emitted by a galaxy at redshift z = 3.794, dubbed Ion1 (Vanzella et al. 2012). The LyC from Ion1 is detected at restframe wavelength λλ 820∼890Å with HST WFC3/UVIS in the F410M band (m 410 = 27.60 ± 0.36 m AB , peak SNR = 4.17 in a circular aperture with radius r = 0.12") and at λλ 700∼830Å with the VLT/VIMOS in the U-band (m U = 27.84 ± 0.19 m AB , peak SNR = 6.7 with a r = 0.6" aperture). A 20-hr VLT/VIMOS spectrum shows low-and high-ionization interstellar metal absorption lines, the P-Cygni profile of C IV and Lyα in absorption. The latter spectral feature differs from what observed in known LyC emitters, which show strong Lyα emission. An HST far-UV color map reveals that the LyC emission escapes from a region of the galaxy that is bluer than the rest, presumably because of lower dust obscuration. The F410M image shows that the centroid of the LyC emission is offset from the centroid of the non-ionizing UV emission by 0.12"±0.03", corresponding to 0.85±0.21 kpc (physical), and that its morphology is likely moderately resolved. These morphological characteristics favor a scenario where the LyC photons produced by massive stars escape from low H I columndensity "cavities" in the ISM, possibly carved by stellar wind and/or supernova. We also collect the VIMOS U-band images of a sample of 107 Lyman-break galaxies with spectroscopic redshifts at 3.40 < z < 3.95, i.e. sampling the LyC, and stack them with inverse-variance weights. No LyC emission is detected in the stacked image, resulting in a 32.5 m AB flux limit (1σ) and an upper limit of absolute LyC escape fraction f abs esc ≤ 0.63%. LyC emitters like Ion1 are very likely at the bright-end of the LyC luminosity function.

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“…The identified knots are shown in Fig. 1, in which A, B and C are same as previous studies (e.g., Adamo et al 2010;Östlin et al 2015;Menacho et al 2021). Furthermore, the smaller star formation knot T (the name is same as the Table 3 of Vader et al (1993)), containing young massive star clusters, is also marked in Fig.…”

Section: Star Formation Knotsmentioning

confidence: 55%

“…In this paper, we focus on the molecular/neutral gas properties of Haro 11, which is a merging system and one of the most extreme starburst BCDs in the nearby universe (e.g., Cormier et al 2012Cormier et al , 2014Östlin et al 2015;Pardy et al 2016;Menacho et al 2019Menacho et al , 2021Östlin et al 2021). The redshift (z) is about 0.0206, collected from the NASA/IPAC Extragalactic Database 1 (NED), corresponding to the distance of 87.2 Mpc and a scale of 420 pc per arc second.…”

Section: Introductionmentioning

confidence: 99%

“…1. These knots are found to contain more than 200 massive star clusters (e.g., Adamo et al 2010;Östlin et al 2015;Menacho et al 2021). Stellar feedback produced by intense starbursts has created outflows and multi-scale structures, such as filaments, arcs and bubbles, which make the merger kinematics much more complex (Menacho et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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The molecular gas resolved by ALMA in the low-metallicity dwarf merging galaxy Haro 11

Gao,

Gu,

Shi

et al. 2022

Preprint

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Context. The physical mechanisms for starburst or quenching in less massive (M * ≤ 10 10 M ) galaxies are unclear. The merger is one of the inescapable processes referred to as both starburst and quenching in massive galaxies. However, the effects of the merger on star formation in dwarf galaxies and their evolution results are still uncertain. Aims. We aim to explore how to trigger and quench star formation in dwarf galaxies by studying the metal-poor gas-rich dwarf mergers based on the multi-band observations at a spatial resolution of ∼ 460 pc. Methods. We use the archival data of ALMA (band 3, 8) and VLT/MUSE to map CO(J =1-0), [CI]( 3 P 1 − 3 P 0 ), and Hα emission in one of the most extreme starburst merging dwarf galaxies, Haro 11. Results. We find the molecular gas is assembled around the central two star-forming regions (knots B and C). The molecular/ionized gas and stellar components show complex kinematics, indicating that the gas is probably at a combined stage of collision of clouds and feedback from star formation. The peak location and distribution of [CI](1-0) strongly resemble the CO(1-0) emission, meaning that it might trace the same molecular gas as CO in such a dwarf merger starburst galaxy. The enhancement of line ratios (∼ 0.5) of [CI]/CO around knot C is probably generated by the dissociation of CO molecules by cosmic rays and far-ultraviolet photons. Globally, Haro 11 and its star-forming regions share similar SFEs as the high-z starburst galaxies or the clumps in nearby (U)LIRGs. Conclusions. Given the high SFE, sSFR, small stellar mass, low metallicity, and deficient HI gas, Haro 11 could be an analog of high-z dwarf starburst and the potential progenitor of the nearby less massive elliptical galaxies. The significantly smaller turbulent pressure and viral parameter will probably trigger the intense starbursts. We also predict that it will quench at M * ≤ 8.5 × 10 9 M .

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Kinematics of Haro 11: The miniature Antennae

Cited by 35 publications

References 67 publications

Haro 11: Where is the Lyman Continuum Source?

Haro 11: Where is the Lyman Continuum Source?

HST Imaging of the Ionizing Radiation from a Star-forming Galaxy at z = 3.794

The molecular gas resolved by ALMA in the low-metallicity dwarf merging galaxy Haro 11

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