Ly<i>α</i> emission in high-redshift galaxies

Tapken, C.; Appenzeller, I.; Noll, Stefan; Richling, Sabine; Heidt, J.; Meinköhn, Erik; Mehlert, D.

doi:10.1051/0004-6361:20065825

Cited by 98 publications

(143 citation statements)

References 61 publications

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“…Additionally, a double peaked Lyα emission line profile was found from the starburst galaxy T1214-277 by Mas-Hesse et al (2003), who concluded that the feature is caused by emission in an outflow. Double-peaked Lyα profiles have been observed also at redshift z ∼ 3, in spectra of star forming galaxies (Fosbury et al 2003;Christensen et al 2004;Venemans et al 2005;Tapken et al 2007).…”

Section: Individual Notesmentioning

confidence: 88%

The great observatories origins deep survey

Vanzella¹,

Cristiani²,

Dickinson

et al. 2007

A&A

335

372

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Aims. We present the full data set of the spectroscopic campaign of the ESO/GOODS program in the GOODS-South field, obtained with the FORS2 spectrograph at the ESO/VLT. Methods. Objects were selected as candidates for VLT/FORS2 observations primarily based on the expectation that the detection and measurement of their spectral features would benefit from the high throughput and spectral resolution of FORS2. The reliability of the redshift estimates is assessed using the redshift-magnitude and color-redshift diagrams, and comparing the results with public data. Results. Including the third part of the spectroscopic campaign (12 masks) to the previous work (26 masks, Vanzella et al. 2005Vanzella et al. , 2006, 1715 spectra of 1225 individual targets have been analyzed. The actual spectroscopic catalog provides 887 redshift determinations. The typical redshift uncertainty is estimated to be σ z 0.001. Galaxies have been selected adopting different color criteria and using photometric redshifts. The resulting redshift distribution typically spans two domains: from z = 0.5 to 2 and z = 3.5 to 6.3. The reduced spectra and the derived redshifts are released to the community through the ESO web page http://www.eso.org/science/goods/.

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Section: Individual Notesmentioning

confidence: 88%

The great observatories origins deep survey

Vanzella¹,

Cristiani²,

Dickinson

et al. 2007

A&A

335

372

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“…Haro 2 also shows an UV continuum luminosity similar to that of the weakest Lyman Break Galaxies (LBGs) in the redshift range z = 2.7−5 (Tapken et al 2007). This fact, together with its high Notes.…”

Section: Introductionmentioning

confidence: 86%

Multiwavelength analysis of the Lyman-αemitting galaxy Haro 2: relation between the diffuse Lyman-αand soft X-ray emissions

Otí-Floranes

Mas-Hesse

Jiménez‐Bailón

et al. 2012

A&A

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Context. Lyman-α emission is commonly used as star formation tracer in cosmological studies. Nevertheless, resonant scattering strongly affects the resulting luminosity, leading to variable and unpredictable escape fractions in different objects. Aims. To understand how the Lyα escape fraction depends on the properties of the star-forming regions, we need high spatial resolution multiwavelength studies of nearby Lyα emitters, like Haro 2. Methods. We study the Lyα emission of Haro 2 in connection with the properties of the young stellar population, the characteristics of the interstellar medium, the distribution and intensity of the Balmer emission lines and the properties of the X-ray emission. We have used HST-STIS spectral images along the major and minor axes of Haro 2 to characterize the Lyα emission, as well as FOC UV, WFPC-2 optical and NICMOS near infrared broadband-filter images to analyze the properties of the stellar population. WFPC-2 Hα image and ground-based spectroscopy allow us to study the Balmer emission lines. Finally, Chandra/ACIS X-ray images provide resolved distribution of the X-ray emission at various energy bands. The observational data are analyzed by comparison with the predictions from evolutionary synthesis models to constrain the properties of the star formation episode. Results. The UV, Hα and far infrared luminosities of the Haro 2 nuclear starburst are well reproduced assuming a young stellar population with ages ∼3.5-5.0 Myr, affected by differential intestellar extinctions. A significant fraction of the stars are completely obscured in the UV, being identifiable only indirectly by their contribution to the ionization of the gas and to the far infrared emission. The diffuse soft X-ray emission extending over the whole source is attributed to gas heated by the mechanical energy released by the starburst. A compact hard X-ray emission (likely an UltraLuminous X-ray source) has been identified in a star-forming condensation to the southeast. Both compact and diffuse Lyα emission components are observed along the major and minor axes in STIS spectral images. Lyα is spatially decoupled from Balmer lines emission, Balmer decrement and UV continuum. However, the diffuse Lyα component is spatially correlated with the diffuse soft X-ray emission. Moreover, unlike the compact Lyα emission, diffuse Lyα shows luminosities larger than predicted from Hα, assuming case B recombination and considering the dust extinction as derived from Hα/Hβ. Conclusions. The Lyα emission closely associated to the massive stellar clusters is strongly affected by the properties of the surrounding neutral gas (presence of outflows, dust abundance), leading to even a range of escape fractions at different locations within the same starburst. On the other hand, we propose that the diffuse Lyα emission originates in gas ionized by the hot plasma responsible for the soft X-ray radiation, as suggested by their spatial correlation and by the measured L(Hα)/L 0.4−2.4 keV ratios. Calibration of Lyα as star forma...

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“…The emission is symmetric, in contrast to the asymmetric line profile characteristic of Lyman break galaxies (LBGs; Tapken et al 2007). This indicates that there is no H i gas in front of the emitting region to absorb the emitted Lyα photons.…”

Section: Position and Profile Of The Emission Linementioning

confidence: 98%

A glance at the host galaxy of high-redshift quasars using strong damped Lyman-αsystems as coronagraphs

Finley

Petitjean

Pâris

et al. 2013

A&A

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We searched quasar spectra from the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) for the rare occurrences where a strong damped Lyman-α absorber (DLA) blocks the Broad Line Region emission from the quasar and acts as a natural coronagraph to reveal narrow Lyα emission from the host galaxy. We define a statistical sample of 31 DLAs in Data Release 9 (DR9) with log N(H i) ≥ 21.3 cm −2 located at less than 1500 km s −1 from the quasar redshift. In 25% (8) of these DLAs, a strong narrow Lyα emission line is observed with flux ∼25 × 10 −17 erg s −1 cm −2 on average. For DLAs without this feature in their troughs, the average 3-σ upper limit is <0.8 × 10 −17 erg s −1 cm −2 . Our statistical sample is nearly 2.5 times larger than the anticipated number of intervening DLAs in DR9 within 1 500 km s −1 of the quasar redshift. We also define a sample of 26 DLAs from DR9 and DR10 with narrow Lyα emission detected and no limit on the H i column density to better characterize properties of the host galaxy emission. Analyzing the statistical sample, we do not find substantial differences in the kinematics, metals, or reddening for the two populations with and without emission detected. The highly symmetric narrow Lyα emission line profile centered in the HI trough indicates that the emitting region is separate from the absorber. The luminosity of the narrow Lyα emission peaks is intermediate between that of Lyα emitters and radio galaxies, implying that the Lyα emission is predominantly due to ionizing radiation from the AGN. Galaxies neighboring the quasar host are likely responsible for the majority (>75%) of these DLAs, with only a minority (<25%) arising from H i clouds located in the AGN host galaxy.

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Lyα emission in high-redshift galaxies

Cited by 98 publications

References 61 publications

The great observatories origins deep survey

The great observatories origins deep survey

Multiwavelength analysis of the Lyman-αemitting galaxy Haro 2: relation between the diffuse Lyman-αand soft X-ray emissions

A glance at the host galaxy of high-redshift quasars using strong damped Lyman-αsystems as coronagraphs

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