Feedback in the Local Lyman‐break Galaxy Analog Haro 11 as Probed by Far‐Ultraviolet and X‐Ray Observations

Grimes, John; Heckman, Timothy M.; Strickland, David; Dixon, W. V.; Sembach, Kenneth R.; Overzier, Roderik; Hoopes, Charles G.; Aloisi, Alessandra; Ptak, Andrew

doi:10.1086/521353

Cited by 106 publications

(157 citation statements)

References 71 publications

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“…This is probably due to a very young stellar population and suggests that stellar winds should be important. A strong superwind [8,43] is observed from the central region and Chandra observations [43] confirm that this wind is penetrating the gaseous halo and may open channels to the halo. In this context it is interesting to compare Haro 11 to high redshift galaxies, in particular Lyman break galaxies [43].…”

Section: Starburstsmentioning

confidence: 73%

Star Forming Dwarf Galaxies

Bergvall¹

2011

Astrophysics and Space Science Proceedings

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Star forming dwarf galaxies (SFDGs) have a high gas content and low metallicities, reminiscent of the basic entities in hierarchical galaxy formation scenarios. In the young universe they probably also played a major role in the cosmic reionization. Their abundant presence in the local volume and their youthful character make them ideal objects for detailed studies of the initial stellar mass function (IMF), fundamental star formation processes and its feedback to the interstellar medium. Occasionally we witness SFDGs involved in extreme starbursts, giving rise to strongly elevated production of super star clusters and global superwinds, mechanisms yet to be explored in more detail. SFDGs is the initial state of all dwarf galaxies and the relation to the environment provides us with a key to how different types of dwarf galaxies are emerging. In this review we will put the emphasis on the exotic starburst phase, as it seems less important for present day galaxy evolution but perhaps fundamental in the initial phase of galaxy formation.

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Section: Starburstsmentioning

confidence: 73%

Star Forming Dwarf Galaxies

Bergvall¹

2011

Astrophysics and Space Science Proceedings

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“…In Bergvall et al (2006), the first actual detection of LyC escape was reported for Haro 11 to be f esc = 4−10%. However, in Grimes et al (2007), the same data set was reduced with a later version of the FUSE pipeline, and here they arrived at contradicting results with f esc 2%. The LyC escape was studied in eight more galaxies from the FUSE archive in Grimes et al (2009).…”

Section: Introductionmentioning

confidence: 80%

“…The shape of the background is therefore pre-determined from those template files. This procedure works satisfactorily for bright targets, but for low S /N spectra the pipeline has been known to overestimate the background at shorter wavelengths producing an unphysical negative flux (seen in e.g., Grimes et al 2007;Grimes et al 2009). Particularly problematic are the SiC 1B and SiC 1A LWRS spectra, because they fall close to the edge of the detectors where the background has a steep slope and is difficult to model properly.…”

Section: Observations Reductions and Data Analysismentioning

confidence: 99%

“…To measure escape fractions and investigate the physical properties that allow leakage, we need to study more nearby objects. This can and has been done with groundbased telescopes at z ∼ 3 (e.g., Steidel et al 2001;Shapley et al 2006;Iwata et al 2009;Vanzella et al 2010;Nestor et al 2011), or locally by using space telescopes such as HUT (Leitherer et al 1995), FUSE (Deharveng et al 2001;Bergvall et al 2006;Grimes et al 2007Grimes et al , 2009, GALEX (Cowie et al 2009), and HST (Malkan et al 2003;Siana et al 2007Siana et al , 2010Bridge et al 2010). Of the four only HST and GALEX are still in operation, and until now only HUT and FUSE have been providing wavelength coverage down to 900 Å, such that local galaxies can be studied.…”

Section: Introductionmentioning

confidence: 99%

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Analyzing low signal-to-noise FUSE spectra

Leitet

Bergvall

Piskunov

et al. 2011

A&A

101

105

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Context. Galaxies are believed to be the main providers of Lyman continuum (LyC) photons during the early phases of the cosmic reionization. Little is known however, when it comes to escape fractions and the mechanisms behind the leakage. To learn more, one may look at local objects, but so far only one low-z galaxy has shown any signs of emitting LyC radiation. With data from the Far Ultraviolet Spectroscopic Explorer (FUSE), we previously found an absolute escape fraction of ionizing photons ( f esc ) of 4-10% for the blue compact galaxy Haro 11. However, using a revised version of the reduction pipeline on the same data set, Grimes and collaborators were unable to confirm this and derived an upper limit of f esc 2% . Aims. We attempt to determine whether Haro 11 is emitting ionizing radiation to a significant level or not. We also investigate the performance of the reduction pipeline for faint targets such as Haro 11, and introduce a new approach to the background subtraction. Methods. The final version of the reduction pipeline, CalFUSE v3.2, was applied to the same Haro 11 data set as the two previous authors used. At these faint flux levels, both FUSE and CalFUSE are pushed to their limits, and a detailed analysis was undertaken to monitor the performance of the pipeline. We show that non-simultaneous background estimates are insuffient when working with data of low signal-to-noise ratio (S /N), and a new background model was developed based on a direct fit to the detector response. Results. We find that one has to be very careful when using CalFUSE v3.2 on low S /N data, and especially when dealing with sources where signal might originate from off-center regions. Applying the new background fit, a significant signal is detected in the LyC in both detector segments covering these wavelengths. Thus, the leakage is confirmed with a flux density of f 900 = 4.0 × 10 −15 erg s −1 cm −2 Å −1 (S /N = 4.6), measured on the airglow free regions in the LyC for the night-only data. This corresponds to an absolute escape fraction of ionizing photons from Haro 11 of f esc = 3.3 ± 0.7%. We confirm these results by investigating the two-dimensional data, the count rates, and the residual flux in C ii λ1036 Å.

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“…It possesses characteristics of an extreme starburst with L FIR ∼ 10 11 L (Sanders et al 2003), making it a luminous infrared galaxy (LIRG) with a high star formation rate of ∼25 M yr −1 as determined from Hα, radio continuum, FIR and hard X-ray observations (Grimes et al 2007). Broadband images of Hα show three bright star-forming condensations with unrelaxed kinematic structure and faint extended shell structures in the outer regions of the galaxy, all suggesting an ongoing merger (Bergvall & Östlin 2002;Östlin et al 1999).…”

Section: The Samplementioning

confidence: 99%

Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz¹,

Madden²,

Galliano³

et al. 2009

A&A

200

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Aims. We study the dust properties of four low metallicity galaxies by modelling their spectral energy distributions. This modelling enables us to constrain the dust properties such as the mass, the temperature or the composition to characterise the global ISM properties in dwarf galaxies. Methods. We present 870 μm images of four low metallicity galaxies (NGC 1705, Haro 11, Mrk 1089 and UM 311) observed with the Large APEX BOlometer CAmera (LABOCA) on the Atacama Pathfinder EXperiment (APEX) telescope. We modeled their spectral energy distributions combining the submm observations of LABOCA, 2MASS, IRAS, Spitzer photometric data, and the IRS data for Haro 11. Results. We found that the PAH mass abundance is very low in these galaxies, 5 to 50 times lower than the PAH mass fraction of our Galaxy. We also found that a significant mass of dust is revealed when using submm constraints compared to that measured with only mid-IR to far-IR observations extending only to 160 μm. For NGC 1705 and Haro 11, an excess in submillimeter wavelengths was detected when we used our standard dust SED model. We rerun our SED procedure adding a cold dust component (10 K) to better describe the high 870 μm flux derived from LABOCA observations, which significantly improves the fit. We found that at least 70% of the dust mass of these two galaxies can reside in a cold dust component. We also showed that the subsequent dust-to-gas mass ratios, considering HI and CO observations, can be strikingly high for Haro 11 in comparison with what is usually expected for these low-metallicity environments. Furthermore, we derived the star formation rate of our galaxies and compared them to the Schmidt law. Haro 11 falls anomalously far from the Schmidt relation. These results may suggest that a reservoir of hidden gas could be present in molecular form not traced by the current CO observations. While there can be a significant cold dust mass found in Haro 11, the SED peaks at exceptionally short wavelengths (36 μm), also highlighting the importance of the much warmer dust component heated by the massive star clusters in Haro 11. We also derived the total IR luminosities derived from our models and compared them with relations that derive this luminosity from Spitzer bands. We found that the Draine & Li (2007) formula compares well to our direct IR determinations.

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Feedback in the Local Lyman‐break Galaxy Analog Haro 11 as Probed by Far‐Ultraviolet and X‐Ray Observations

Cited by 106 publications

References 71 publications

Star Forming Dwarf Galaxies

Star Forming Dwarf Galaxies

Analyzing low signal-to-noise FUSE spectra

Probing the dust properties of galaxies up to submillimetre wavelengths

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