adsabs/AstroCLIMB huggingface dataset:
Paper: Robust Estimates of Orientation between Astrometric Catalogs
Authors: Julien Frouard
Figure caption: A simple linear regression problem schematically representing the differences between one random realization from the synthetic simulations discussed in Section 3 (left) and the real data treated in Section 4 (right). See text for explanations.
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: Sky coverage of the six DEIMOS masks (gray shade) in the SSA22-Sb1 field. All spectroscopic targets for the SSA22-HIT survey are superposed by their categories: T1 (2.7 < z ex < 3.2) in cyan filled circles, T2 (3.2 < z ex < 3.7) in green filled circles, T3 (3.7 < z ex < 4.5) in red filled circles, T4 (4.3 < z ex < 4.8) in magenta filled circles, T5 (4.8 < z ex < 5.6) in brown filled circles, LyCs by x-marks, SMGs by open triangles, oldLAE by an asterisk, LAEs in the low-density region (LDRLAEs) by open squares, z = 3.1 protocluster members (PCs) by open pentagons, and the galaxy sight-line DLA and its counterpart candidates (galDLAs) by crosses. The background contours show the smoothed number density of the z = 3.1 LAEs: 0.5 (dashed), 1 (thick), 2, 3, 4, and 5 times the average density (0.2 arcmin−2; Yamada et al. 2012b).
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: Two color diagrams used to select the spectroscopic targets in the five categories: T1, T2, T3, T4, and T5. In individual panels, the red solid (dotted) lines correspond to the color tracks of the Bruzual & Charlot (2003) galaxy models from z = 0–7 with constant star formation history, stellar age of 100 Myr, and dust extinctions of E(B − V) = 0 (0.25). The boundary redshifts of the categories are represented by squares. The brown dotted–dashed lines are also the Bruzual & Charlot (2003) model tracks but with instantaneous star formation history, stellar age of 1 Gyr, and no dust extinction. The model galaxies are dominated by the mature stellar population. The colors of Galactic stars from the Pickles (1998) library are shown by green triangles. The blue circles correspond to the observed galaxies whose redshifts are spectroscopically confirmed to be in the redshift range of each category (Steidel et al. 2003; Kousai 2011; Saez et al. 2015; Hayashino et al. 2019). The arrows indicate the 2σ limits for nondetections in the bands at wavelengths shorter than the Lyman break. Our target selection criteria are shown in the gray shaded regions.
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: Observed spectra of four example galaxies taken with the Keck/DEIMOS in the SSA22-HIT survey. The four galaxies are sorted by their redshift quality flags. In each figure, the one-dimensional (top panel) and two-dimensional (bottom panel) spectra are shown. The black and gray lines correspond to the one-dimensional spectra and error spectra that are smoothed with a 5 pixel box-car kernel, respectively. We also show much more smoothed spectra with a 39 pixel box-car kernel using the red lines. The yellow shaded region corresponds to the wavelength range in which we analyze the foreground H I Lyα absorption. The green shaded regions represent the atmospheric absorption bands. The vertical dashed lines represent the wavelengths of the possible emission/absorption lines. The blue arrows superimposed on the two-dimensional spectra mark the lines that were visually identified.
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: Spectroscopic redshift distribution of the objects identified in the SSA22-HIT survey by the redshift quality flags (top) and the target categories (bottom). The objects that show low-z contamination at 0 ≤ z ≤ 0.5 are shown in the subpanels. The two-headed arrows represent the expected redshift ranges of the five major target categories (T1, T2, T3, T4, and T5).
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: Sky distributions of the objects observed in the SSA22-HIT survey. All targets observed are shown by open circles, while the filled circles correspond to the objects whose redshifts are determined (z < 3.2 in cyan, 3.05 ≤ z ≤ 3.12 in blue, 3.2 ≤ z < 3.7 in green, 3.7 ≤ z < 4.5 in red, and z ≥ 4.5 in brown). The background contours show the z = 3.1 LAE number density, which are the same as those in Figure 3.
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: (Bottom) Magnitude distribution of all targets (black solid) and objects spectroscopically confirmed (gray shaded) in the SSA22-HIT survey. We used the ﹩i^{\prime} ﹩-band magnitudes. Because some of the T4 and T5 category targets and SMGs were not detected in the ﹩i^{\prime} ﹩ band, we used the ﹩z^{\prime} ﹩-band magnitudes for them. The spectroscopically confirmed objects were divided by their redshift quality flags. (Top) Number fraction of spectroscopically confirmed objects over all targets.
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: Transmissions of the filters used in the target selection (blue: u*, purple: B, dark-green: V, orange: R  c , magenta: ﹩i^{\prime} ﹩, red: ﹩z^{\prime} ﹩, cyan: NB359, light-green: NB497, and yellow: NB816) together with model spectra of star-forming galaxies at z = 3.0, 3.5, 4.0, 4.6, and 5.2 from the Bruzual & Charlot (2003) library (gray lines).