The CGM and IGM at z ∼ 5: metal budget and physical connection

Codoreanu, Alex; Ryan-Weber, E. V.; Crighton, Neil H. M.; Becker, George D.; Madau, Piero; Venemans, Bram

doi:10.1093/mnras/sty2576

Cited by 39 publications

(68 citation statements)

References 78 publications

(112 reference statements)

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“…This limiting column density allows them to study the identified SiIV population across the column density range [12.5, 14.0] over the full redshift path of their survey. In addition, Codoreanu et al (2018) show that the fiducial configuration in García et al (2017b) at z = 5.6 is compatible with the SiIV observations.…”

Section: Introductionsupporting

confidence: 80%

“…The calculated CDDFs are always below the observed values, and for high column densities, there is a clear departure from the fitting functions provided by D' Odorico et al (2013). Nonetheless, the synthetic CDDFs have a closer match with the observational values from Codoreanu et al (2018), in particular at high column densities. It is worth noting that Bosman et al (2017) data are just upper limits for the CIV-CDDF at 6.2 < z < 7.0, nevertheless the computed values in this test are significantly underrepresented.…”

Section: Change In the Normalization Of Hm12supporting

confidence: 55%

“…with m ion the mass of the ionic species, n lov is the number of lines of view, ρ crit is the critical density today and ∆X is expressed above. Figure 5 shows a comparison of the calculated CIV cosmological mass density at 4 < z < 8 for synthetic absorbers in the range 13.8 < (log N CIV / cm −2 ) < 15.0 and observations by Pettini et al (2003) and Ryan-Weber et al (2009) in orange circles, Codoreanu et al (2018) in yellow circles, Songaila et al (2001Songaila et al ( , 2005 remarkable difference is visible in the reference run Ch 18 512 MDW, with an order of magnitude shift between the blue curve (on the left) and the light blue one (on the right). Therefore, strong variations of the UVB around 1 Ryd (specifically, normalization changes in the wavelength range where the transition occurs) seem to have a large impact on the number of CIV absorbers at all redshifts.…”

Section: Change In the Normalization Of Hm12mentioning

confidence: 99%

“…CIV cosmological mass density at 4 < z < 8 for 13.8 < log N CIV (cm −2 ) < 15.0. Comparison between the simulated data and observations byPettini et al (2003) andRyan-Weber et al (2009) in orange circles,Codoreanu et al (2018) in yellow circles,Songaila et al (2001Songaila et al ( , 2005 in cyan triangles,Meyer et al (2019) in magenta triangles,Simcoe et al (2011) in dark green inverted triangles, D'Odorico et al (2013) in pink squares,Boksenberg et al (2015) in grey diamond, upper limits fromBosman et al (2017) in purple star andDíaz et al (2016) in black pentagons. Pettini, Ryan-Weber, Codoreanu and Díaz measurements are converted to the Planck cosmology, while for the others this recalibration was not possible due to missing details of the precise pathlength probed.…”

mentioning

confidence: 94%

“…Alternatively, intervening metal absorption lines detected in the spectra of high redshift quasars offer a completely different method to calibrate the UVB at high redshift. A growing number of absorption systems has been detected (Bosman et al 2017;Codoreanu et al 2018;Meyer et al 2019;Becker et al 2019) and with the advent of bigger telescopes (e.g. GMT), the expectation is that the sample of absorption lines detected significantly increases.…”

Section: Introductionmentioning

confidence: 99%

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Can Uvb Variations Reconcile Simulated Quasar Absorption Lines at High Redshift?

Ryan-Weber

2020

RMxAA

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RESUMENEn este trabajo, presentamos nuevos resultados de los observables asociados a líneas de absorción sintéticas de HI y metales en el espectro de cuásares a alto redshift, inspirados por preguntas y limitaciones encontradas en un trabajo previo con el fondo ionizante uniforme (UVB) de Haard-Madau 2012. Introducimos variaciones del fondo ionizante y el modelo de self-shielding del Hidrógeno neutro y exploramos la sensibilidad de las líneas de absorción al modificar la intensidad del UVB. Encontramos que los estados de baja ionización (por ejemplo, CII, SiII, OI) y SiIV están bien representadas por un UV ionizante más suave, pero este mismo modelo falla en reproducir las propiedades estadísticas de la población observada de CIV. Por esto, recomendamos una reducción moderada de la emisividad del fondo ionizante a este redshift, un order de magnitud por debajo. De otro lado, variaciones en el self-shielding de HI dejan un marca en la función de distribución de las columnas de densidad en HI a z = 4 y en la densidad de masa cósmica en el rango de 4 < z < 6. Concluimos que pequeñas variaciones en el fondo de UV y en el apantallamiento de Hidrógeno neutro a z ∼ 6 juegan un papel importante en el mejoramiento de la estimación de las estadísticas de metales y HI a este redshift. ABSTRACTIn this work, we present new calculations of the observables associated with synthetic metal and HI absorption lines in the spectra of high redshift quasars, inspired by questions and limitations raised in work with a uniform Haardt-Madau 2012 ultraviolet background (UVB). We introduce variations at z ∼ 6 to the UVB and HI self-shielding and explore the sensitivity of the absorption features to modifications of the hardness of the UVB. We find that observed SiIV and low ionization states (e.g. CII, SiII, OI) are well represented by a soft UV ionizing field at z = 6 but, this same prescription, fails to reproduce the statistical properties of the observed ion CIV absorber population. Therefore, we recommend a moderate reduction of the UVB at this redshift, an emissivity change between the UVB models that lies in between the Haardt-Madau 2012 emissivity J ν and one with a dex below J ν − 1 at 1 Ryd. On the other hand, variations in the HI self-shielding (SSh) prescription leave a non-negligible

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Section: Introductionsupporting

confidence: 80%

Section: Change In the Normalization Of Hm12supporting

confidence: 55%

Section: Change In the Normalization Of Hm12mentioning

confidence: 99%

mentioning

confidence: 94%

Section: Introductionmentioning

confidence: 99%

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Can Uvb Variations Reconcile Simulated Quasar Absorption Lines at High Redshift?

Ryan-Weber

2020

RMxAA

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Compact [C ii] emitters around a C iv absorption complex at redshift 5.7

Kashino

Lilly

Simcoe

et al. 2023

Nature

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The physical conditions of the circumgalactic medium are probed by intervening absorption-line systems in the spectrum of background quasistellar objects out to the epoch of cosmic reionization [1][2][3][4]. A correlation between the ionization state of the absorbing gas and the nature of the nearby galaxies has been suggested by the sources detected either in Lyα or [C ii] 158 µm near to respectively highly-ionized and neutral absorbers [5,6]. This is also likely linked to the global changes in the incidence of absorption systems of different types and the process of cosmic reionization [7][8][9][10][11][12]. Here we report the detection of two [C ii]-emitting galaxies at redshift z ≈ 5.7 that are associated with a

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X-Shooting ULLYSES: Massive stars at low metallicity

Sana,

Tramper,

Abdul-Masih

et al. 2024

A&A

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Context. The XShootU project aims to obtain ground-based optical to near-infrared spectroscopy of all targets observed by the Hubble Space Telescope (HST) under the Director’s Discretionary program ULLYSES. Using the medium-resolution spectrograph X-shooter, spectra of 235 OB and Wolf-Rayet (WR) stars in subsolar metallicity environments have been secured. The bulk of the targets belong to the Large and Small Magellanic Clouds, with the exception of three stars in NGC 3109 and Sextans A. Aims. This second paper in the series focuses on the optical observations of Magellanic Clouds targets. It describes the uniform reduction of the UVB (300–560 nm) and VIS (550–1020 nm) XShootU data as well as the preparation of advanced data products that are suitable for homogeneous scientific analyses. Methods. The data reduction of the RAW data is based on the ESO CPL X-shooter pipeline. We paid particular attention to the determination of the response curves. This required equal flat-fielding of the science and flux standard star data and the derivation of improved flux standard models. The pipeline products were then processed with our own set of routines to produce a series of advanced data products. In particular, we implemented slit-loss correction, absolute flux calibration, (semi-)automatic rectification to the continuum, and a correction for telluric lines. The spectra of individual epochs were further corrected for the barycentric motion, re-sampled and co-added, and the spectra from the two arms were merged into a single flux-calibrated spectrum covering the entire optical range with maximum signal-to-noise ratio. Results. We identify and describe an undocumented recurrent ghost visible on the RAW data. We present an improved flat-fielding strategy that limits artifacts when the SCIENCE and FLUX standard stars are observed on different nights. The improved FLUX standard models and the new grid of anchor points limit artifacts of the response curve correction, for example on the shape of the wings of the Balmer lines, from a couple of per cent of the continuum level to less than 0.5%. We confirm the presence of a radial velocity shift of about 3.5 km s−1 between the UVB and the VIS arm of X-shooter and that there are no short term variations impacting the RV measurements. RV precision better than 1 km s-1 can be obtained on sharp telluric lines while RV precision on the order of 2 to 3 km s-1 is obtained on data with the best S/N. Conclusions. For each target observed by XShootU, we provide three types of data products: (i) two-dimensional spectra for each UVB and VIS exposure before and after correction for the instrument response; (ii) one-dimensional UVB and VIS spectra as produced by the X-shooter pipeline before and after response-correction, and applying various processing, including absolute flux calibration, telluric removal, normalization and barycentric correction; and (iii) co-added flux-calibrated and rectified spectra over the full optical range, for which all available XShootU exposures were combined. For the large majority of the targets, the final signal-to-noise ratio per resolution element is above 200 in the UVB and in the VIS co-added spectra. The reduced data and advanced scientific data products are made available to the community. Together with the HST UV ULLYSES data, they should enable various science goals, from detailed stellar atmosphere and stellar wind studies, and empirical libraries for population synthesis, to the study of the local nebular environment and feedback of massive stars in subsolar metallicity environments.

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The CGM and IGM at z ∼ 5: metal budget and physical connection

Cited by 39 publications

References 78 publications

Can Uvb Variations Reconcile Simulated Quasar Absorption Lines at High Redshift?

Can Uvb Variations Reconcile Simulated Quasar Absorption Lines at High Redshift?

Compact [C ii] emitters around a C iv absorption complex at redshift 5.7

X-Shooting ULLYSES: Massive stars at low metallicity

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