First Detection of Na<scp>i</scp>D Lines in High‐Redshift Damped Lyα Systems

Kondo, Sohei; Kobayashi, Naoto; Minowa, Yosuke; Tsujimoto, Takuji; Churchill, Christopher W.; Takato, Naruhisa; Iye, Masanori; Kamata, Yukiko; Terada, Hiroshi; Pyo, Tae‐Soo; Takami, Hideki; Hayano, Yutaka; Kanzawa, Tomio; Saint-Jacques, David; Gäessler, Wolfgang; Oya, Shin; Nedachi, Ko; Tokunaga, A. T.

doi:10.1086/502960

Cited by 6 publications

(6 citation statements)

References 54 publications

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“…This shows that cold material is entrained and expelled outside the disc by the ionized gas flow. In this context, the findings of Kondo et al (2006), York et al (2006) and Wild et al (2006) are very interesting. For the first time, Kondo et al detected strong Na i Dλλ5891/5897 doublet absorption in two strong Mg ii absorbers (also DLAs) at z abs = 1.062 & 1.18 towards the gravitationally lensed QSO APM 08279+5255.…”

Section: Physical Interpretationmentioning

confidence: 83%

New perspectives on strong z≃ 0.5 Mg ii absorbers: are halo mass and equivalent width anticorrelated?

Bouché

Murphy

Péroux

et al. 2006

Monthly Notices of the Royal Astronomical Society

146

221

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We measure the mean halo-mass of z ≃ 0.5 Mg II absorbers using the cross-correlation (over co-moving scales 0.05-13h −1 Mpc) between 1806 Mg II quasar absorption systems and ∼ 250,000 Luminous Red Galaxies (LRGs), both selected from the Sloan Digital Sky Survey Data Release 3. The Mg II systems have λ2796 rest-frame equivalent widths W λ2796 r 0.3Å. From the ratio of the Mg II-LRG cross-correlation to the LRG-LRG auto-correlation, we find that the bias ratio between Mg II absorbers and LRGs is b Mg II /b LRG = 0.65 ± 0.08, which implies that the absorber host-galaxies have a mean halo-mass ∼ 20-40 times smaller than that of the LRGs; the Mg II absorbers have haloes of mean mass log M h (M ⊙ ) = 11.94 ± 0.31(stat) +0.24 −0.25 (sys). We demonstrate that this statistical technique, which does not require any spectroscopic follow-up, does not suffer from contaminants such as stars or foreground and background galaxies. Finally, we find that the absorber halo-mass is anticorrelated with the equivalent width. If Mg II absorbers were virialized in galaxy haloes a positive M h -W λ2796 r correlation would have been observed since W λ2796 r is a direct measure of the velocity spread of the Mg II sub-components. Thus, our results demonstrate that the individual clouds of a Mg II system are not virialized in the gaseous haloes of the host-galaxies. We review past results in the literature on the statistics of Mg II absorbers and find that they too require an M h -W λ2796 r anti-correlation. When combined with measurements of the equivalent width distribution (d 2 N/dz/dW r ), the M h -W λ2796 r anti-correlation naturally explains why absorbers with W λ2796 r 2Å are not seen at large impact parameters. We interpret the M h -W λ2796 r anti-correlation within the starburst scenario where strong Mg II absorbers are produced by supernovae-driven winds.

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Section: Physical Interpretationmentioning

confidence: 83%

New perspectives on strong z≃ 0.5 Mg ii absorbers: are halo mass and equivalent width anticorrelated?

Bouché

Murphy

Péroux

et al. 2006

Monthly Notices of the Royal Astronomical Society

146

221

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“…To study the degree of dust depletion in the absorbers, the N Na i /N Ca ii ratio has often been used as a probe (Welsh et al 1990;Bertin et al 1993;Crawford et al 2002;Kondo et al 2006), because sodium is hardly depleted onto grains while calcium can be strongly depleted (Savage & Sembach 1996).…”

Section: Possible Association With Known Ivc or Hvc Complexesmentioning

confidence: 99%

“…19 column density ratios as a function of log N Na i . Three other data sets were kindly provided by Sohei Kondo (see also Kondo et al 2006). The red symbols show damped Lyman α (DLA) data (1.06 ≤ z ≤ 1.18) obtained by Kondo et al (2006) with the near-infrared instrument IRCS (Infrared Camera and Spectrograph) installed at the Subaru Telescope.…”

Section: Possible Association With Known Ivc or Hvc Complexesmentioning

confidence: 99%

“…Three other data sets were kindly provided by Sohei Kondo (see also Kondo et al 2006). The red symbols show damped Lyman α (DLA) data (1.06 ≤ z ≤ 1.18) obtained by Kondo et al (2006) with the near-infrared instrument IRCS (Infrared Camera and Spectrograph) installed at the Subaru Telescope. Black circles show the data for the Milky Way by Vallerga et al (1993) who observed Ca ii and Na i absorbers towards 46 early type stars in the local ISM with distances between d = 20 .…”

Section: Possible Association With Known Ivc or Hvc Complexesmentioning

confidence: 99%

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An absorption-selected survey of neutral gas in the Milky Way halo

Bekhti

Winkel

Richter

et al. 2012

A&A

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Aims. We aim at analysing systematically the distribution and physical properties of neutral and mildly ionised gas in the Milky Way halo, based on a large absorption-selected data set. Methods.Multi-wavelength studies were performed combining optical absorption line data of Ca ii and Na i with follow-up H i 21-cm emission line observations along 408 sight lines towards low-and high-redshift QSOs. We made use of archival optical spectra obtained with UVES/VLT. H i data were extracted from the Effelsberg-Bonn H i survey and the Galactic All-Sky survey.For selected sight lines we obtained deeper follow-up observations using the Effelsberg 100-m telescope.Results. Ca ii (Na i) halo absorbers at intermediate and high radial velocities are present in 40-55% (20-35%) of the sightlines, depending on the column density threshold chosen. Many halo absorbers show multi-component absorption lines, indicating the presence of sub-structure. In 65% of the cases, absorption is associated with H i 21-cm emission. The Ca ii (Na i) column density distribution function follows a power-law with a slope of β ≈ −2.2 (−1.4). Conclusions. Our absorption-selected survey confirms our previous results that the Milky Way halo is filled with a large number of neutral gas structures whose high column density tail represents the population of common H i high-and intermediate-velocity clouds seen in 21-cm observations. We find that Na i/Ca ii column density ratios in the halo absorbers are typically smaller than those in the Milky Way disc, in the gas in the Magellanic Clouds, and in damped Lyman α systems. The small ratios (prominent in particular in high-velocity components) indicate a lower level of Ca depletion onto dust grains in Milky Way halo absorbers compared to gas in discs and inner regions of galaxies.

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“…The Na I and Ca II abundances have been studied in the Galaxy and LMC (Hunter et al 2006;Vladilo et al 1993). Beyond the Local Group, Na I and Ca II have been detected in 2 damped Lyman-α systems (DLAs) in QSO spectra, at z = 1.062 and 1.181 (Petitjean et al 2000;Kondo et al 2006). Other QSO absorption line studies report upper limits for Na I (Boksenberg et al 1978;1980).…”

Section: Absorption Lines In the Circumburst Mediummentioning

confidence: 99%

The nature of the dwarf starforming galaxy associated with GRB 060218/SN 2006aj

Wiersema¹,

Savaglio

Vreeswijk

et al. 2007

A&A

112

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Context. We present high resolution VLT UVES and low resolution FORS optical spectroscopy of supernova 2006aj and its host galaxy, associated with the nearby (z = 0.03342) gamma-ray burst GRB 060218. This host galaxy is a unique case, as it is one of the few nearby GRB host galaxies known, and it is only the second time high resolution spectra have been taken of a nearby GRB host galaxy (after GRB 980425). Aims. The resolution, wavelength range and S/N of the UVES spectrum combined with low resolution FORS spectra allow a detailed analysis of the circumburst and host galaxy environments. Methods. We analyse the emission and absorption lines in the spectrum, combining the high resolution UVES spectrum with low resolution FORS spectra and find the metallicity and chemical abundances in the host. We probe the geometry of the host by studying the emission line profiles.Results. Our spectral analysis shows that the star forming region in the host is metal poor with 12 + log(O/H) = 7.54 +0.17 −0.10 (∼0.07 Z ), placing it among the most metal deficient subset of emission-line galaxies. It is also the lowest metallicity found so far for a GRB host from an emission-line analysis. Given the stellar mass of the galaxy of ∼10 7 M and the SFR Hα = 0.065 ± 0.005 M yr −1 , the high specific star formation rate indicates an age for the galaxy of less than ∼200 Myr. The brightest emission lines are clearly asymmetric and are well fit by two Gaussian components separated by ∼22 km s −1 . We detect two discrete Na i and Ca ii absorption components at the same redshifts as the emission components. We tentatively interpret the two components as arising from two different starforming regions in the host, but high resolution imaging is necessary to confirm this.

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First Detection of NaiD Lines in High‐Redshift Damped Lyα Systems

Cited by 6 publications

References 54 publications

New perspectives on strong z≃ 0.5 Mg ii absorbers: are halo mass and equivalent width anticorrelated?

New perspectives on strong z≃ 0.5 Mg ii absorbers: are halo mass and equivalent width anticorrelated?

An absorption-selected survey of neutral gas in the Milky Way halo

The nature of the dwarf starforming galaxy associated with GRB 060218/SN 2006aj

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