Detection of emission lines from<i>z</i>∼ 3 DLAs towards the QSO J2358+0149

Srianand, R.; Hussain, Tanvir; Noterdaeme, P.; Petitjean, P.; Krühler, T.; Japelj, J.; Pâris, Isabelle; Kashikawa, Nobunari

doi:10.1093/mnras/stw951

Cited by 33 publications

(34 citation statements)

References 108 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We derive the star-formation rate (SFR) of this candidate based on the Lyα flux (FLyα = 1.9 × 10 −17 erg s −1 cm −2 , that corresponds to the Lyα luminosity of LLyα = 7.7 × 10 41 erg s −1 ) using the Kennicutt (1998) relation. The derived SF R of 0.7 M⊙ yr −1 is a bit lower than other detection of DLA counterparts at z > 2 reported by some previous studies (e.g., Fumagalli et al 2010;Péroux et al 2012;Bouché et al 2013;Fynbo et al 2013;Krogager et al 2013;Srianand et al 2016). …”

Section: A Candidate Of a Dla Counterpartcontrasting

confidence: 67%

“…Since DLAs dominate the neutral-gas content in a wide redshift range (Storrie-Lombardi & Wolfe 2005), they are thought to be gas reservoirs for the starformation in the high-z Universe. Though the DLA is such an important population, their nature is still under the debate (e.g., Prochaska & Wolfe 1997;Taniguchi & Shioya 2000;2001;Kacprzak et al 2010) because it is often difficult to identify their optical counterparts due to their faintness, especially at high redshift (see for recent identifications at z > 2, Fynbo et al 2010;2011;Péroux et al 2011;Bouché et al 2013;Krogager et al 2012, Kashikawa et al 2014, Srianand et al 2016Sommer-Larsen & Fynbo 2017 and references therein). In many cases, counterparts of high-z DLAs have been found as LAEs.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A search for Ly α emitters around a concentrated region of strong Ly α absorbers at z = 2.3

Ogura

Nagao

Imanishi

et al. 2017

Publications of the Astronomical Society of Japan

Self Cite

View full text Add to dashboard Cite

In order to investigate the physical relationship between strong Lyα absorbers (logN HI ≥ 20.0 cm −2 ) such as damped Lyα absorption systems (DLAs) and young star-forming galaxies at high redshift, we have conducted narrow-band observations of Lyα emitters (LAEs) in a concentrated region of strong Lyα absorbers at z = 2.3, the J1230+34 field. Using a catalog of Lyα absorbers with logN HI ≥ 20.0 cm −2 based on the baryon oscillation spectroscopic survey (BOSS), we found 6 fields where 3 or more absorbers are concentrated within a (50 Mpc) 3 cubic box in the comoving scale. Among them, we focus on the J1230+34 field, where 2 DLAs and 2 sub-DLAs present. Our narrow-band imaging observations with Subaru/Suprime-Cam using a custom-made filter, N B400 (λ c = 4003Å and FWHM= 92Å) yield a sample of 149 LAEs in this field. In the large scale (∼50 Mpc), we have found no differences between the obtained Lyα luminosity function and those in the blank fields at similar redshifts. We also compare the frequency distribution of the Lyα rest-frame equivalent width (EW 0 ) in the target field and other fields including both overdensity region and blank field, but find no differences. On the other hand, in the small scale (∼10 Mpc), we have found a possible overdensity of LAEs around a DLA with the highest H I column density (N HI = 21.08 cm −2 ) in the target field while there are no density excess around the other absorbers with a lower N HI .

show abstract

Section: A Candidate Of a Dla Counterpartcontrasting

confidence: 67%

Section: Introductionmentioning

confidence: 99%

A search for Ly α emitters around a concentrated region of strong Ly α absorbers at z = 2.3

Ogura

Nagao

Imanishi

et al. 2017

Publications of the Astronomical Society of Japan

Self Cite

View full text Add to dashboard Cite

show abstract

“…Cen 2012;Bird et al 2014) or semi-analytical models (e.g. Berry et al 2016) but direct associations with galaxies remain difficult to establish, with only a few associations between intervening DLAs and galaxies revealed so far at z > 2 (Møller & Warren 1993;Møller et al 2004;Fynbo et al 2010;Krogager et al 2012;Noterdaeme et al 2012b;Bouché et al 2013;Kashikawa et al 2014;Hartoog et al 2015;Srianand et al 2016). Indeed, statistical studies show a low level of in-situ star formation (Rahmani et al 2010;Fumagalli et al 2015), although Ly-α emission has been detected through stacking in sub-samples with the highest H i column densities , suggesting the latter arise more likely from gas associated with galaxies at small impact parameters.…”

Section: Introductionmentioning

confidence: 99%

Discovery of a Perseus-like cloud in the early Universe

Noterdaeme

Krogager

Balashev

et al. 2017

A&A

View full text Add to dashboard Cite

We present the discovery of a molecular cloud at z abs ≈ 2.5255 along the line of sight to the quasar SDSS J 000015.17+004833.3. We use a high-resolution spectrum obtained with the Ultraviolet and Visual Echelle Spectrograph together with a deep multi-wavelength medium-resolution spectrum obtained with X-shooter (both on the Very Large Telescope) to perform a detailed analysis of the absorption lines from ionic, neutral atomic and molecular species in different excitation levels, as well as the broad-band dust extinction.We find that the absorber classifies as a Damped Lyman-α system (DLA) with log N(H i) (cm −2 ) = 20.8 ± 0.1. The DLA has supersolar metallicity (Z ∼ 2.5 Z , albeit to within a factor of two to three) with a depletion pattern typical of cold gas and an overall molecular fraction f = 2N(H 2 )/(2N(H 2 ) + N(H i)) ∼ 50%. This is the highest f -value observed to date in a high-z intervening system. Most of the molecular hydrogen arises from a clearly identified narrow (b ∼ 0.7 km s −1 ), cold component in which carbon monoxide molecules are also found, with log N(CO) ≈ 15. With the help of the spectral synthesis code Cloudy, we study the chemical and physical conditions in the cold gas. We find that the line of sight probes the gas deep after the H i-to-H 2 transition in a ∼4−5 pc-size cloud with volumic density n H ∼ 80 cm −3 and temperature of only 50 K. Our model suggests that the presence of small dust grains (down to about 0.001 µm) and high cosmic ray ionisation rate (ζ H ∼ a few times 10 −15 s −1 ) are needed to explain the observed atomic and molecular abundances. The presence of small grains is also in agreement with the observed steep extinction curve that also features a 2175 Å bump. Interestingly, the chemical and physical properties of this cloud are very similar to what is seen in diffuse molecular regions of the nearby Perseus complex, despite the former being observed when the Universe was only 2.5 Gyr old. The high excitation temperature of CO rotational levels towards J0000+0048 betrays however the higher temperature of the cosmic microwave background. Using the derived physical conditions, we correct for a small contribution (0.3 K) of collisional excitation and obtain T CMB (z = 2.53) ≈ 9.6 K, in perfect agreement with the predicted adiabatic cooling of the Universe.

show abstract

“…In contrast, the detected galactic counterparts to z > 2 DLAs unsurprisingly represent a biased sample; the galaxies typically have significantly higher SFRs, and on average, the metallicity of the DLAs is higher (Fynbo et al 2010;Péroux et al 2012;Fumagalli et al 2015) Fumagalli et al (2015) recently reviewed the published results and found that only 11 z > 1.9, log(N HI ) > 20.3 absorption systems were known to have galactic counterparts at the same spectroscopically identified redshift (Møller & Warren 1993;Møller et al 2002Møller et al , 2004Weatherley et al 2005;Fynbo et al 2010Fynbo et al , 2011Bouché et al 2012;Krogager et al 2012;Noterdaeme et al 2012b;Péroux et al 2013;Bouché et al 2013;Jorgenson & Wolfe 2014). Since 2015, at least five additional plausible host galaxies have been identified (Hartoog et al 2015;Srianand et al 2016;Neeleman et al 2017). In addition to these, a handful of high-z sub-DLAs with 19.0 < log(N HI ) < 20.3 have identified nearby galaxies (c.f.…”

Section: Introductionmentioning

confidence: 99%

A Unique View of AGN-driven Molecular Outflows: The Discovery of a Massive Galaxy Counterpart to a Z = 2.4 High-metallicity Damped Lyα Absorber

Rudie

Newman

Murphy

2017

ApJ

View full text Add to dashboard Cite

We report the discovery of a massive log(M/M ⊙ ) = 10.74 +0.18−0.16 galaxy at the same redshift as a carbon-monoxide-bearing sub-damped Lyman α absorber (sub-DLA) seen in the spectrum of QSO J1439+1117. The galaxy, J1439B, is located 4.′′ 7 from the QSO sightline, a projected distance of 38 physical kpc at z = 2.4189, and exhibits broad optical emission lines (σ [OIII] = 303 ± 12 km s −1 ) with ratios characteristic of excitation by an active galactic nucleus (AGN). The galaxy has a factor of ∼9 lower star formation than is typical of star-forming galaxies of the same mass and redshift. The nearby sub-DLA is highly enriched, suggesting its galactic counterpart must be massive if it follows the z ∼ 2 mass-metallicity relationship. Metallic absorption within the circumgalactic medium of the sub-DLA and J1439B is spread over a velocity range ∆v > 1000 km s −1 , suggesting an energetic origin. We explore the possibility that a different galaxy could be responsible for the rare absorber, and conclude that it is unlikely based on imaging, integral-field spectroscopy, and high-z massive galaxy pair statistics. We argue that the gas seen in absorption against the QSO was likely ejected from the galaxy J1439B and therefore provides a unique observational probe of AGN feedback in the distant universe.

show abstract

Detection of emission lines fromz∼ 3 DLAs towards the QSO J2358+0149

Cited by 33 publications

References 108 publications

A search for Ly α emitters around a concentrated region of strong Ly α absorbers at z = 2.3

A search for Ly α emitters around a concentrated region of strong Ly α absorbers at z = 2.3

Discovery of a Perseus-like cloud in the early Universe

A Unique View of AGN-driven Molecular Outflows: The Discovery of a Massive Galaxy Counterpart to a Z = 2.4 High-metallicity Damped Lyα Absorber

Contact Info

Product

Resources

About