adsabs/AstroCLIMB huggingface dataset:
Paper: UVCANDELS: Catalogs of Photometric Redshifts and Galaxy Physical Properties
Authors: Vihang Mehta, Marc Rafelski, Ben Sunnquist, Harry I. Teplitz, Claudia Scarlata, Xin Wang, Adriano Fontana, Nimish P. Hathi, Kartheik G. Iyer, Anahita Alavi, James Colbert, Norman Grogin, Anton Koekemoer, Kalina V. Nedkova, Matthew Hayes, Laura Prichard, Brian Siana, Brent M. Smith, Rogier Windhorst, Teresa Ashcraft, Micaela Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Adam Broussard, Timothy Carleton, Nima Chartab, Alex Codoreanu, Seth Cohen, Christopher Conselice, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, Duilia De Mello, Mark Dickinson, Najmeh Emami, Henry Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven Finkelstein, Jonathan P. Gardner, Eric Gawiser, Timothy Gburek, Mauro Giavalisco, Andrea Grazian, Caryl Gronwall, Yicheng Guo, Pablo Arrabal Haro, Shoubaneh Hemmati, Justin Howell, Rolf A. Jansen, Zhiyuan Ji, Sugata Kaviraj, Keunho J. Kim, Peter Kurczynski, Ilin Lazar, Ray A. Lucas, John MacKenty, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Bahram Mobasher, Alexa M. Morales, Robert O'Connell, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Michael Rutkowski, Brant Robertson, Zahra Sattari, Emmaris Soto, Lei Sun, Sina Taamoli, Eros Vanzella, L. Y. Aaron Yung, Bonnabelle Zabelle
Figure caption: An aggregate comparison between the photometric and spectroscopic redshifts for all four CANDELS fields combined. The left panels show the comparison where all available filters were included in the photometric-redshift fitting, where as the right panels show the same without using filters from the UVCANDELS program (i.e., F275W/F435W for COSMOS and EGS; F275W for GOODS-N and GOODS-S). The top panels include all sources, where as the bottom panels only show sources with multiple peaks in their probability distributions P(z) and with SNR > 3 in F275W. The improvement of the photometric redshift by including the UV photometry is evident in this case, reducing both σ NMAD and η for sources detected in the UV or that previously had multiple peaks in P(z).
Paper: UVCANDELS: Catalogs of Photometric Redshifts and Galaxy Physical Properties
Authors: Vihang Mehta, Marc Rafelski, Ben Sunnquist, Harry I. Teplitz, Claudia Scarlata, Xin Wang, Adriano Fontana, Nimish P. Hathi, Kartheik G. Iyer, Anahita Alavi, James Colbert, Norman Grogin, Anton Koekemoer, Kalina V. Nedkova, Matthew Hayes, Laura Prichard, Brian Siana, Brent M. Smith, Rogier Windhorst, Teresa Ashcraft, Micaela Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Adam Broussard, Timothy Carleton, Nima Chartab, Alex Codoreanu, Seth Cohen, Christopher Conselice, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, Duilia De Mello, Mark Dickinson, Najmeh Emami, Henry Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven Finkelstein, Jonathan P. Gardner, Eric Gawiser, Timothy Gburek, Mauro Giavalisco, Andrea Grazian, Caryl Gronwall, Yicheng Guo, Pablo Arrabal Haro, Shoubaneh Hemmati, Justin Howell, Rolf A. Jansen, Zhiyuan Ji, Sugata Kaviraj, Keunho J. Kim, Peter Kurczynski, Ilin Lazar, Ray A. Lucas, John MacKenty, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Bahram Mobasher, Alexa M. Morales, Robert O'Connell, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Michael Rutkowski, Brant Robertson, Zahra Sattari, Emmaris Soto, Lei Sun, Sina Taamoli, Eros Vanzella, L. Y. Aaron Yung, Bonnabelle Zabelle
Figure caption: The SED modeling shown for an example galaxy (GOODS-N-26886). The top-left panel shows the observed photometry (shown in blue) along with the best-fit model template from the flexible (DENSE BASIS, in red) and fixed (CIGALE, in green) SFH assumptions. The insets show 5″ × 5″ postage stamps of the galaxy in the respective filters. The bottom-left panel shows the best-fit SFH for both cases demonstrating how the flexible-form SFH captures star formation at earlier times that is missed by the fixed-form approach, while both return an excellent overall fit to the observed photometry. For the DENSE BASIS result, a corner plot with the posterior distributions of the free parameters is shown on the right along with the best-fit parameter values for both cases.
Paper: UVCANDELS: Catalogs of Photometric Redshifts and Galaxy Physical Properties
Authors: Vihang Mehta, Marc Rafelski, Ben Sunnquist, Harry I. Teplitz, Claudia Scarlata, Xin Wang, Adriano Fontana, Nimish P. Hathi, Kartheik G. Iyer, Anahita Alavi, James Colbert, Norman Grogin, Anton Koekemoer, Kalina V. Nedkova, Matthew Hayes, Laura Prichard, Brian Siana, Brent M. Smith, Rogier Windhorst, Teresa Ashcraft, Micaela Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Adam Broussard, Timothy Carleton, Nima Chartab, Alex Codoreanu, Seth Cohen, Christopher Conselice, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, Duilia De Mello, Mark Dickinson, Najmeh Emami, Henry Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven Finkelstein, Jonathan P. Gardner, Eric Gawiser, Timothy Gburek, Mauro Giavalisco, Andrea Grazian, Caryl Gronwall, Yicheng Guo, Pablo Arrabal Haro, Shoubaneh Hemmati, Justin Howell, Rolf A. Jansen, Zhiyuan Ji, Sugata Kaviraj, Keunho J. Kim, Peter Kurczynski, Ilin Lazar, Ray A. Lucas, John MacKenty, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Bahram Mobasher, Alexa M. Morales, Robert O'Connell, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Michael Rutkowski, Brant Robertson, Zahra Sattari, Emmaris Soto, Lei Sun, Sina Taamoli, Eros Vanzella, L. Y. Aaron Yung, Bonnabelle Zabelle
Figure caption: An example of the photometric-redshift probability distribution combination process for an example source (COSMOS-697: z spec = 1.6418; z phot = 1.61 ± 0.05). Blue curves show the P(z)s from the individual codes, orange curves show these P(z)s after smoothing, and the black curves show the final combined P(z) before (dashed) and after (solid) the final sharpening procedure. The final photometric redshift (cross symbol) and confidence intervals (shaded gray region) of the final P(z) are shown, along with the spectroscopic redshift (dotted line).
Paper: UVCANDELS: Catalogs of Photometric Redshifts and Galaxy Physical Properties
Authors: Vihang Mehta, Marc Rafelski, Ben Sunnquist, Harry I. Teplitz, Claudia Scarlata, Xin Wang, Adriano Fontana, Nimish P. Hathi, Kartheik G. Iyer, Anahita Alavi, James Colbert, Norman Grogin, Anton Koekemoer, Kalina V. Nedkova, Matthew Hayes, Laura Prichard, Brian Siana, Brent M. Smith, Rogier Windhorst, Teresa Ashcraft, Micaela Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Adam Broussard, Timothy Carleton, Nima Chartab, Alex Codoreanu, Seth Cohen, Christopher Conselice, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, Duilia De Mello, Mark Dickinson, Najmeh Emami, Henry Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven Finkelstein, Jonathan P. Gardner, Eric Gawiser, Timothy Gburek, Mauro Giavalisco, Andrea Grazian, Caryl Gronwall, Yicheng Guo, Pablo Arrabal Haro, Shoubaneh Hemmati, Justin Howell, Rolf A. Jansen, Zhiyuan Ji, Sugata Kaviraj, Keunho J. Kim, Peter Kurczynski, Ilin Lazar, Ray A. Lucas, John MacKenty, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Bahram Mobasher, Alexa M. Morales, Robert O'Connell, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Michael Rutkowski, Brant Robertson, Zahra Sattari, Emmaris Soto, Lei Sun, Sina Taamoli, Eros Vanzella, L. Y. Aaron Yung, Bonnabelle Zabelle
Figure caption: Comparison of the performance of the photometric redshifts with the spectroscopic sample for each of the individual fields. The key statistics, i.e., the scatter (σ NMAD) and the outlier fraction (η = ∣Δz∣/(1 + z) > 0.15) are reported in the upper left corner. The inset shows the distribution of the fractional differences between the photometric and spectroscopic redshifts. The dotted lines show the outlier criterion: z phot = z spec ± 0.15(1 + z spec) and the dashed lines show the median of the distribution.
Paper: UVCANDELS: Catalogs of Photometric Redshifts and Galaxy Physical Properties
Authors: Vihang Mehta, Marc Rafelski, Ben Sunnquist, Harry I. Teplitz, Claudia Scarlata, Xin Wang, Adriano Fontana, Nimish P. Hathi, Kartheik G. Iyer, Anahita Alavi, James Colbert, Norman Grogin, Anton Koekemoer, Kalina V. Nedkova, Matthew Hayes, Laura Prichard, Brian Siana, Brent M. Smith, Rogier Windhorst, Teresa Ashcraft, Micaela Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Adam Broussard, Timothy Carleton, Nima Chartab, Alex Codoreanu, Seth Cohen, Christopher Conselice, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, Duilia De Mello, Mark Dickinson, Najmeh Emami, Henry Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven Finkelstein, Jonathan P. Gardner, Eric Gawiser, Timothy Gburek, Mauro Giavalisco, Andrea Grazian, Caryl Gronwall, Yicheng Guo, Pablo Arrabal Haro, Shoubaneh Hemmati, Justin Howell, Rolf A. Jansen, Zhiyuan Ji, Sugata Kaviraj, Keunho J. Kim, Peter Kurczynski, Ilin Lazar, Ray A. Lucas, John MacKenty, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Bahram Mobasher, Alexa M. Morales, Robert O'Connell, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Michael Rutkowski, Brant Robertson, Zahra Sattari, Emmaris Soto, Lei Sun, Sina Taamoli, Eros Vanzella, L. Y. Aaron Yung, Bonnabelle Zabelle
Figure caption: The mass distribution as a function of redshift for each field, with the masses estimated using the flexible (DENSE BASIS, left panel) and fixed (CIGALE, right panel) SFH assumptions.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Combined constraints of hidden planets from our TTV analysis of 260 hot Jupiter systems. The color of each grid point indicates the percentage of hot Jupiter systems within our sample that can hide companion planets with the corresponding planet mass and period ratio. The three solid lines represent equal-percentage lines near 10%, 50%, and 90%, respectively. The left panel shows the results from the χ 2 method, while the right panel displays the results from the rms test. The masses of Earth, Neptune, and Jupiter are marked with dashed lines.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: The median upper mass limit of the hidden companions near resonances 1:2, 2:1, and 3:1 is expressed in Earth masses. The orbital period (P) and radius (R  p ) of the primary planets are categorized into 15 × 5 bins, with the bins for the orbital period logarithmically spaced. The yellow numbers represent the number of systems in each bin. The color coding indicates the median maximum mass limit of the hidden companions.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: The red dashed line and white line represent the upper mass limit of a possible companion around WASP-142 b, calculated by χ 2 and rms analysis, respectively. The background color represents the mean exponential growth factor of nearby orbits (MEGNO) calculated from the rebound simulation, which helps us assess the dynamical stability of the simulated planetary system. The MEGNO value is a measure of chaos in a dynamical system, with 〈Y〉 converging to 2 indicating a stable system.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: The graph displays the TTVs extracted from a linear model of WASP-142 b. The blue line represents the TTVs obtained from two separate observation data sets, while the yellow line shows a zoomed-in view for each observation. The total rms of all observations is 40 seconds, with individual observations having an rms of 43 and 36 s, respectively.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Corner plot derived from the MCMC fitting of WASP-142 b’s orbital parameters. This plot specifically illustrates the transit midtime, orbital period, square of the radius ratio, star density, and impact factor from our result.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Same as Figure 7, but for hot Jupiter systems with known companion planets, namely WASP-84 b, WASP-132 b and WASP-47 b.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Distribution of transit number for 260 hot Jupiter systems. The majority of systems have less than 100 transits, while some of them have more than 200 transits.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Flowchart of our TTV analysis method.
Paper: Constraining the Presence of Companion Planets in Hot Jupiter Planetary Systems Using Transit-timing Variation Observations from TESS
Authors: Zixin Zhang, Wenqin Wang, Xinyue Ma, Zhangliang Chen, Yonghao Wang, Cong Yu, Shangfei Liu, Yang Gao, Baitian Tang, Bo Ma
Figure caption: Cumulative probability of the rms of TTVs calculated from TESS observation data for our sample of 260 hot Jupiter systems.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Violin plot representations of velocity dispersion (a), excitation temperature (b), effective radius (c), mass (d), surface density (e), number density (f), viral parameter (g), and internal pressure (h) for the clouds within each Galactocentric radial bins of 1 kpc. The upper panel shows raw categories, while the bottom panel presents statistics for the filtered categories (refer to Section 3.2 for details). Violin plots are histograms, where the width along the x-axis indicates the normalized fraction of data at the corresponding y-axis value. Blue lines within the violins extend from the minimum to the maximum of the distributions. Squares and circles represent the median and mean of the property distributions, respectively. The fitting results for maximum and mean values are labeled in the bottom panel of each property as dotted and dashed lines, respectively. To better illustrate the changing tendency of mean values with R GC, we add a zoomed-in secondary y-axis, overlaying mean values as red circles on the right y-axis. Note that the scale range of the y-axis is fixed for each property.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Relationships between mass and effective radius for the full sample and the different subsamples, including the unresolved and resolved, and the resolved clouds located in different distances from the Galactic center. For example, the subsample “R GC < 10.5 kpc” comprises all resolved clouds within the Galactocentric distance less than 10.5 kpc. The green shadings, ﹩M(r)\leqslant 870\,{M}_{\odot }{\left(R/\mathrm{pc}\right)}^{1.33}﹩, denote the regions where interstellar clouds are deemed insufficiently massive to foster high-mass star formation (e.g., J. Kauffmann et al. 2010). The fitting results are also annotated in each graph, with the Spearman's rank correlation coefficients marked in parentheses. The colors on the points represent the distribution of the probability density functions of the cloud counts (2D probability density functions), which are calculated by utilizing kernel density estimation through Gaussian kernels in the Python package scipy.stats.Gaussian_kde. The black dotted lines indicate the result of the CfA survey from MD+2017.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Relationships between virial parameter and mass of MCs. The sample is the same as Figure 6. The pink shadings indicate the regions of α vir ≤ 2. Each panel also labeled the fractions of total mass, and total number (in the parenthesis) of structures that satisfy α vir ≤ 2. The red solid lines delineate the log-log linear least-squares fitting relations between the physical properties. The black dotted lines indicate the result of the CfA survey from MD+2017.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Relationships between velocity dispersion and effective radius of MCs. The sample is the same as Figure 6. The first Larson’s relation revealed by the inner Galaxy MCs from P. M. Solomon et al. (1987) and the entire disk MCs from MD+2017 are also drawn with the black dashed and dotted lines for comparison. For better comparison, the orange contours show the kernel density estimate of the distribution for cloud groups presented in the right column are overlaid in both the middle and left columns.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Cumulative distributions of effective radius (R eff), and mass (M) for the MCs. Comparisons are made among the entire cloud sample and subsamples in different R GC components. The dotted lines indicate the minimum meaningful value of each property. A nontruncated power-law spectrum is fitted to each distribution above the meaningful value, and the resulting index for each distribution is labeled.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Violin plot representations of excitation temperature (a) and mass (b) for clouds within each 1 kpc Galactocentric radial bin, after the correction of beam-filling factor and sensitivity-clip factor, respectively.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Same as Figure 6 but considering the variation of X CO with R GC. The dashed-red and solid-red lines represent the fitting results based on constant and variable X CO, respectively.
Paper: Molecular Clouds in the Outer Milky Way Disk: Sample, Integrated Properties, and Radial Trends with Galactocentric Radius
Authors: Yan Sun, Ji Yang, Qing-Zeng Yan, Shaobo Zhang, Yang Su, Xuepeng Chen, Xin Zhou, Yuehui Ma, Lixia Yuan
Figure caption: Surface density of molecular gas mass for Galactic radii ranging from 9 to 20 kpc. The black and blue lines are the fit to the data before and after applying the flux completeness correction. The orange dotted line is from MD+2017, their yielded fitting for the CfA catalog in the 4 < R GC < 17 kpc range.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Upper panels: Lyα line map (left) and g-band image (right) of the field around Ivory Nebula. The line map reveals the extremely extended Lyα emission of the enormous Lyα nebula. The 2σ surface brightness limit is ﹩7.76\times {10}^{-18}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{\mathrm{arcsec}}^{-2}﹩. Cyan and white lines represent the 2σ and 5σ Lyα contours, respectively. Yellow lines denote the long slit to take spectra. Lower left panel: 2D and 1D spectra of the Ivory Nebula. The 2D spectrum shows the spatial extent of Lyα emission along the slit (oriented along the yellow lines in the upper right). 1D spectra were extracted using fixed-width apertures corresponding to the three components labeled (components A, B, and C). The spectra reveal complicated Lyα line profiles and the detection of N V doublet emission in component A. Lower right panel: composite RGB image (g band in red and NB400 in blue) of the ELAN pair composed of Ivory Nebula and MLAN10. Pixels with values of <2σ rms are set in black color. The projected angular separation between these two ELANe is about 1′.
Paper: MAMMOTH-Subaru. II. Diverse Populations of Circumgalactic Lyα Nebulae at Cosmic Noon
Authors: Mingyu Li, 明宇 李, Haibin Zhang, Zheng Cai, Yongming Liang, Nobunari Kashikawa, Ke Ma, Xiaohui Fan, J. Xavier Prochaska, Bjorn H. C. Emonts, Xin Wang, Yunjing Wu, Shiwu Zhang, Qiong Li, Sean D. Johnson, Minghao Yue, Fabrizio Arrigoni Battaia, Sebastiano Cantalupo, Joseph F. Hennawi, Satoshi Kikuta, Yuanhang Ning, Masami Ouchi, Rhythm Shimakawa, Ben Wang, Weichen Wang, Zheng Zheng, Zhen-Ya Zheng
Figure caption: Diagnosis of Type II ELANe (>100 kpc) with UV-faint (M UV > −22) host galaxies. Type II ELANe are the majority (∼80%) in the population of ELANe. The x-axis is the rest-frame absolute UV magnitude. The y-axis denotes the projected Lyα angular size. The size of each circle denotes the diffuse Lyα isophotal area. The color of each circle denotes the Lyα luminosity. The UV magnitude distribution of ELANe is shown in the upper panel with a bimodal feature. Type II ELANe are located in the upper left corner with a faint UV continuum but widespread Lyα emissions, while Type I ELANe are located at the upper right of this figure with a strong UV continuum. The background of this figure is colored just for visual distinction. The largest six nebulae in this work are labeled, and all are Type II nebulae. For summary and comparison, a few Type II nebulae reported in previous literature are drawn as hexagons in this figure, including MAMMOTH-1 (Z. Cai et al. 2017a; S. Zhang et al. 2023b) and SSA22-LAB1, SSA22-LAB2 (C. C. Steidel et al. 2000; Y. Matsuda et al. 2004). QSO confirmed by spectroscopic observations (blue cross), radio galaxies (green diamond), and IR-luminous DOGs (blue plus sign) are overlaid on the figure.