Erratum: Deep VLT spectroscopy of the $\vec{z}=$ 2.49 radio galaxy MRC 2104-242

Overzier, Roderik; Röttgering, H. J. A.; Kurk, J.; Breuck, C. De

doi:10.1051/0004-6361:20010436

Cited by 10 publications

(14 citation statements)

References 6 publications

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“…Our detection of the quiescent Lyα halo of 2104−242 (Overzier et al 2001; Villar‐Martín et al 2003) in the light of [O iii ]λ5008 and Hα shows that this halo is ionized, and is not merely neutral gas acting as a Lyα mirror. Similarly, by way of detection of [O ii ]λ3728, [O iii ]λ5008 and Hα, we have shown that the giant Lyα halo of 4C+10.48 (see van Ojik et al 1997) is ionized.…”

Section: Discussionmentioning

confidence: 85%

“…We suggest that He ii λ1640/Hβ can be used to make a first order estimate of A v when Hα/Hβ and He ii λ1640/He ii λ4687 are not available. In addition, we have identified several new line ratios to calculate electron temperature: [Ne v ]λ1575/[Ne v ]λ3426, [Ne iv ]λ1602/[Ne iv ]λ2423, O iii ]λ1663/[O iii ]λ5008 and [O ii ]λ2471/[O ii ]λ3728. Using O iii ]λ1663/[O iii ]λ5008 we have calculated an average T e of 14100 +1000 −600 K. Our detection of the quiescent Lyα halo of 2104−242 (Overzier et al 2001; Villar‐Martín et al 2003) in the light of [O iii ]λ5008 and Hα shows that this halo is ionized, and is not merely neutral gas acting as a Lyα mirror. Similarly, by way of detection of [O ii ]λ3728, [O iii ]λ5008 and Hα, we have shown that the giant Lyα halo of 4C+10.48 (see van Ojik et al 1997) is ionized.…”

Section: Discussionmentioning

confidence: 89%

“…Both 4C+10.48 and 2104−242 show two distinct knots of line emission close to the continuum centroid, and in both cases we extracted a spectrum for each knot. When coadded, the two apertures for 2104−242 correspond to the northern extraction aperture used for the optical spectrum by Overzier et al (2001). The one‐dimensional (1D) NIR spectra are shown in Figs 1–3.…”

Section: Observations and Datamentioning

confidence: 99%

“…Rest‐frame optical line spectra for sources meeting these criteria were taken from Motohara et al (2001), Egami et al (2003) and Iwamuro et al (2003), and the rest‐frame UV line spectra are from Röttgering et al (1997), Overzier et al (2001) and Broderick et al (2007).…”

Section: Observations and Datamentioning

confidence: 99%

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Deep spectroscopy of the FUV-optical emission lines from a sample of radio galaxies at z 2.5: metallicity and ionization

Humphrey

Villar-Martı́n

Vernet

et al. 2008

Monthly Notices of the Royal Astronomical Society

148

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We present long‐slit near‐infrared (NIR) spectra, obtained using the Infrared Spectrometer And Array Camera (ISAAC) instrument at the Very Large Telescope, which sample the rest‐frame optical emission lines from nine radio galaxies at z∼ 2.5. One‐dimensional spectra have been extracted and, using broad‐band photometry, have been cross‐calibrated with spectra from the literature to produce line spectra spanning a rest wavelength of ∼1200–7000 Å. The resulting line spectra have a spectral coverage that is unprecedented for radio galaxies at any redshift. We have also produced a composite of the rest‐frame ultraviolet (UV)–optical line fluxes of powerful, z∼ 2.5 radio galaxies. We have investigated the relative strengths of Lyα, Hβ, Hα, He iiλ1640 and He iiλ4687, and we find that Av can vary significantly from object to object. In addition, we have identified new line ratios to calculate electron temperature: [Ne v]λ1575/[Ne v]λ3426, [Ne iv]λ1602/[Ne iv]λ2423, O iii]λ1663/[O iii]λ5008 and [O ii]λ2471/[O ii]λ3728. We calculate an average O iii temperature of 14100+1000−600 K. We have modelled the rich emission line spectra, and we conclude that they are best explained by active galactic nucleus (AGN) photoionization with the ionization parameter U varying between objects. For shock models (with or without the precursor) to provide a satisfactory explanation for the data, an additional source of ionizing photons is required – presumably the ionizing radiation field of the AGN. Single slab photoionization models are unable to reproduce the high‐ and the low‐ionization lines simultaneously: the higher ionization lines imply higher U than do the lower ionization lines. This problem may be alleviated either by combining two or more single slab photoionization models with different U, or by using mixed‐medium models such as those of Binette, Wilson & Storchi‐Bergmann. In either case, U must vary from object to object. On the basis of N v/N iv] and N iv]/C iv we argue that, while photoionization is the dominant ionization mechanism in the extended emission line regions (EELR), shocks make a fractional contribution (∼10 per cent) to its ionization. The N v/N iv] and N iv]/C iv ratios in the broad‐line region (BLR) of some quasars suggest that shock ionization may be important in the BLR also. We find that in the EELR of z∼ 2 radio galaxies the N/H abundance ratio is close to its solar value. We conclude that N/H and metallicity do not vary by more than a factor of 2 in our sample. These results are consistent with the idea that the massive ellipticals which become the hosts to powerful AGN are assembled very early in the history of the universe, and then evolve relatively passively up to the present day.

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Section: Discussionmentioning

confidence: 85%

Section: Discussionmentioning

confidence: 89%

Section: Observations and Datamentioning

confidence: 99%

Section: Observations and Datamentioning

confidence: 99%

See 2 more Smart Citations

Deep spectroscopy of the FUV-optical emission lines from a sample of radio galaxies at z 2.5: metallicity and ionization

Humphrey

Villar-Martı́n

Vernet

et al. 2008

Monthly Notices of the Royal Astronomical Society

148

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“…Another possibility is that the Lyα emission arises from gas associated with the debris of massive mergers that is being illuminated by the AGN (Yajima et al, 2013;Yang et al, 2014;Hennawi et al, 2015;Johnson et al, 2015). Lyα halos and LABs often show substantial chemical enrichment (De Breuck et al, 2000;Overzier et al, 2001;Prochaska & Hennawi, 2009;Hennawi et al, 2015), which would perhaps be most easily explained by the outflow or merger scenario, rather than a scenario where the gas originates from the IGM.…”

Section: Protoclusters and Lyα Blobsmentioning

confidence: 99%

The realm of the galaxy protoclusters

Overzier

2016

Astron Astrophys Rev

279

204

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The study of galaxy protoclusters is beginning to fill in unknown details of the important phase of the assembly of clusters and cluster galaxies. This review describes the current status of this field and highlights promising recent findings related to galaxy formation in the densest regions of the early universe. We discuss the main search techniques and the characteristic properties of protoclusters in observations and simulations, and show that protoclusters will have present-day masses similar to galaxy clusters when fully collapsed. We discuss the physical properties of galaxies in protoclusters, including (proto-)brightest cluster galaxies, and the forming red sequence. We highlight the fact that the most massive halos at high redshift are found in protoclusters, making these objects uniquely suited for testing important recent models of galaxy formation. We show that galaxies in protoclusters should be among the first galaxies at high redshift making the transition from a gas cooling regime dominated by cold streams to a regime dominated by hot intracluster gas, which could be tested observationally. We also discuss the possible connections between protoclusters and radio galaxies, quasars, and Ly-alpha blobs. Because of their early formation, large spatial sizes and high total star formation rates, protoclusters have also likely played a crucial role during the epoch of reionization, which can be tested with future experiments that will map the neutral and ionized cosmic web. Last, we review a number of promising observational projects that are expected to make significant impact in this growing, exciting field.Comment: Invited article for The Astronomy and Astrophysics Review (in press

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The giant Lyα nebula associated with a z = 2.5 radio galaxy

et al. 2006

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Abstract. We present a kinematic and morphological study of the giant Lyα nebula associated with the radio galaxy MRC 2104−242 (z = 2.49) based on integral field spectroscopic VIMOS data from VLT. The galaxy appears to be embedded in a giant ( > ∼ 120 kpc) gas reservoir that surrounds it completely. The kinematic properties of the nebula suggest that it is a rotating structure, which would imply a lower limit to the dynamical mass of ∼ 3 × 10 11 M . An alternate scenario is that the gas is infalling. Such a process would be able to initiate and sustain significant central starburst activity, although it is likely to contribute with less than 10% of the total stellar mass of the galaxy.

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Erratum: Deep VLT spectroscopy of the $\vec{z}=$ 2.49 radio galaxy MRC 2104-242

Cited by 10 publications

References 6 publications

Deep spectroscopy of the FUV-optical emission lines from a sample of radio galaxies at z 2.5: metallicity and ionization

Deep spectroscopy of the FUV-optical emission lines from a sample of radio galaxies at z 2.5: metallicity and ionization

The realm of the galaxy protoclusters

The giant Lyα nebula associated with a z = 2.5 radio galaxy

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