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4 results for “protoclusters”
Characterizing protoclusters and protogroups at z∼2.5 using Lyman-α Tomography (data repo)
<p><strong>Data repo</strong> : Characterizing protoclusters and protogroups at z∼2.5 using Lyman-α Tomography :</p> <p>The generated data in <a href="https://ui.adsabs.harvard.edu/abs/2022ApJ...930..109Q/abstract">Qezlou et. al. 2021</a> </p> <p>Guide on how to use the data :</p> <ul> <li>This data is used by this package (<a href="https://doi.org/10.5281/zenodo.6133235">Zenodo</a> or <a href="https://github.com/mahdiqezlou/LyTomo-Watershed">GitHub</a> ). </li> <li>Feel free to download only the relevant data you need. Refer to <a href="https://github.com/mahdiqezlou/LyTomo-Watershed/blob/main/CookBook.ipynb">this cook book</a> and all the other referred notebooks to see which data file you need to download for each task. </li> <li>There is a module in our package to download these files with python. See <a href="https://github.com/mahdiqezlou/LyTomo_Watershed#generated-data">this</a>.</li> </ul> <ul> <li>Below we provide a short description on each compressed file and the data inside it. </li> </ul> <p> </p> <ol> <li>./descendants/ : Containing data related to the z=0 descendants of the structures (aka. watersheds ) in mock-observed maps at z=2.5.</li> <li>./DM_Density_field/ : Holds the DM density field of the TNG snapshots at z= 2.3, 2=.245, 2.6</li> <li>./FGPA/ : Data generated for the noiseless FGPA map or used to test FGPA accuracy.</li> <li>./mock_maps_z*/ : 20 mock maps generated for each redshift snapshot</li> <li>./noiseless_maps/ : noiseless \delta_F maps for different redshifts</li> <li>./plotting_data/ : summary data used to make plotting easier</li> <li>./progenitor_maps/ : The density maps at z=2.5 for progenitor DM particles of all z=0 halos with M(z=0) > 10^13.5 M_\{odot}/h</li> <li>./progenitors/ : Summary data for progenitors. e.g cofm and a list of their z=0 halo mass</li> <li>./purenoise_maps/ : pure noise maps. Added noise on flat spectra (F = <F>) and then Wiener filtered. </li> <li>./spectra_z*/ : holding extracted spectra from TNG-Illustris snapshots. They are noise free and it will be added in the next step of the analysis. Please, refer to our <a href="https://github.com/mahdiqezlou/LyTomo_Watershed/blob/main/notebooks/CookBook.ipynb">cook book</a></li> <li>./watersheds_z*/ : The watersheds found in all mock maps and noiseless maps at 3 different redshifts. </li> </ol> <p> </p> <p>If you have any questions please feel free to reach mea via email : mahdi.qezlou@email.ucr.edu or raise and issue <a href="https://github.com/mahdiqezlou/LyTomo-Watershed/issues">on our code repository</a>:</p>
Galaxy groups and protocluster candidates in the CLAUDS and HSC-SSP joint deep surveys
<p>Using the extended halo-based group finder developed by <a href="http://iopscience.iop.org/article/10.3847/1538-4357/abddb2/pdf">Yang et al. 2021</a>, which is able to deal with galaxies via spectroscopic and photometric redshifts simultaneously, we (<a href="http://arxiv.org/abs/2205.05517">Li et al. 2022</a>) construct galaxy group and candidate protocluster catalogs in a wide redshift range (<span class="math-tex">\(0 < z < 6\)</span>) from the joint CFHT Large Area <em>U</em>-band Deep Survey (CLAUDS) and Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) deep data set. Based on a selection of 5,607,052 galaxies with<em> i</em>-band magnitude m<em><sub>i </sub></em>< 26 and a sky coverage of 34.41 deg<sup>2</sup>, we identify a total of 2,232,134 groups, within which 402,947 groups have at least three member galaxies. By checking the galaxy number distributions within a 5-7 <em>h<sup>-1</sup></em>Mpc projected separation and a redshift difference <span class="math-tex">\(\Delta z \leq 0.1\)</span> around those richest groups at redshift <span class="math-tex">\(z > 2\)</span>, we identified a list of 761, 343 and 43 protocluster candidates in the redshift bins <span class="math-tex">\(2 \leq z < 3\)</span>, <span class="math-tex">\(3 \leq z < 4\)</span> and <span class="math-tex">\(z > 4\)</span>, respectively. </p> <p> </p> <p>More details can be found in our paper (<a href="http://arxiv.org/abs/2205.05517">arXiv: 2205.05517</a>). Our catalogs are also shared at <a href="http://gax.sjtu.edu.cn/data/PFS.html">https://gax.sjtu.edu.cn/data/PFS.html</a>.</p>
POSITIVE AGN FEEDBACK AT HUNDREDS OF KPC SCALES IN A PROTOCLUSTER AT Z=1.7
<p>High-z protoclusters are ideal laboratories to investigate the relation between AGN feedback, ICM heating, and galaxy evolution at the peak formation epoch of galaxy clusters.</p> <p>We will present multi-band observations of a z=1.7 protocluster assembling around an FRII radio-galaxy that provide strong insight into the above processes.</p> <p>A deep (0.5 Ms) Chandra look at the system revealed several spots of diffuse X-ray emission, the most prominent of which (bubble A) overlaps with the Eastern radio lobe. We will discuss thermal emission or Inverse Compton scattering of CMB photons (IC-CMB) as viable mechanisms to produce the observed X-ray spots, and present new LOFAR observations suggesting that bubble A is due to IC-CMB. In addition, the expanding plasma in the Western radio-jet and lobe likely shock-heats pockets of gas in the inhomogeneous ambient medium to the ~keV temperature observed in the other X-ray spots.</p> <p>Bubble A is surrounded by the four galaxies with the largest specific star formation rates among all protocluster members. This calls for remarkable, positive AGN feedback produced hundreds of kpc away from the FRII nucleus by the expanding bubble.</p> <p>We will discuss future observations of the system and finally present prospects for future population studies of similar, high-z protoclusters with the Survey and Time-domain Astrophysical Research eXplorer (STAR-X), a Medium Explorer mission selected by NASA for Phase A study.</p> <p> </p>
Figure Sets, Catalog Tables, and Other Technical Materials Related to "ALMA-IMF IX: Catalog and Physical Properties of 315 SiO Outflow Candidates in 15 Massive Protoclusters"
<p>This Zenodo DOI contains additional data products and technical files for the publication "ALMA-IMF IX: Catalog and Physical Properties of 315 SiO Outflow Candidates in 15 Massive Protoclusters" (Towner et al. 2024).</p> <p>All files, metadata, and other components and materials in this Zenodo entry are licensed under Creative Commons license CC-BY-NC 4.0. This license allows for non-commercial use so long as proper attribution is given to the original creator. Commercial use of these materials is prohibited. Further details of this license can be found on the Creative Commons website at: https://creativecommons.org/licenses/by-nc/4.0/ </p> <p> </p> <p>This upload contains:</p> <p>1. The Figure Set for Figure 1. The .png summary figures are contained in 5 zip files (Figset1_part1of5.zip, etc.). The file naming structure is <fieldname>_<candididatename>.summary.png, i.e. the summary figure for Candidate #1 in Field G008.67 is G008.67_s1.summary.png.</p> <p>2. The Figure Set for Figure C1. All 15 .png files are contained in the file "FigsetD1_all.zip." Please note: due to post-acceptance edits at the proofing stage, there is no Appendix D in the ApJ article. All files with "D1" in the name refer to either Figure Set C1 or Table C1 in the ApJ publication, as appropriate. </p> <p>3. ECSV versions of Table 3 and Table C1 (labeled as "D1" in this upload), and a LaTeX version of Table 3.</p> <p>4. CRTF apertures and position-velocity paths for all candidates, and FITS files of the position-velocity diagrams for all candidates. The relevant file is "apertures_paths_pvdiagrams.zip." This file contains a directory structure. There are 15 subdirectories, each named for the field to which it corresponds. Within each subdirectory are the aperture and pvpath CRTF files, and the PV diagram FITS files. </p> <p> a. Apertures follow the naming convention s??_aperture.crtf, where "??" is the candidate number. Apertures are color-coded by outflow color (red outflows use red lines, blue outflows use blue, and bipolar outflows use purple/magenta). The aperture for G008.67 Candidate #1 is named s1_aperture.crtf, etc.</p> <p> b. Position-velocity paths follow the naming convention "s??_path<.direction>.crtf" where <.direction> is ".ra" or ".dec" or blank (""). Directions are necessary because CARTA saves point-like regions in the order in which they were last modified. In order to ensure the points are used in the correct order in pvextractor (or another program), users should first sort the points in the CRTF file in order of increasing ra (for files containing ".ra") or increasing dec (for files containing ".dec"). Files without a <.direction> in the name indicate that the candidate is classified as "complex or cluster" and so sorting is not particularly relevant. </p> <p> c. Position-velocity diagrams are uploaded as FITS files, and follow the naming convention "s??_pvslice.fits" where "??" is the candidate number. Note that some paths are extremely short and thus their PV diagrams can be difficult to read. Although all PV diagrams are shown as square in Towner et al. (2024), allowing the PV diagram to display with its natural aspect ratio may be more useful in some cases.</p> <p> </p> <p>Final note:</p> <p>The FITS cubes used in this analysis are not uploaded to Zenodo due to upload size limitations. The full cubes and continuum images for each field can be found on the ALMA-IMF Project website (https://www.almaimf.com/data.html). Cubes cut to +/- 95 km/s, noise cubes, and cubes in units of K instead of Jy/beam can be requested by emailing Dr. Allison Towner at apmtowner [at] gmail.com.</p>
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