adsabs/AstroCLIMB huggingface dataset:
Paper: Warped Disk Galaxies. II. From the Cosmic Web to the Galactic Warp
Authors: Woong-Bae G. Zee, S. Lyla Jung, Sanjaya Paudel, Suk-Jin Yoon
Figure caption: Upper: probability density function, P(ϕ), of satellite PA, ϕ, relative to the major axis of the central galaxy, for unwarped control sample (left, black), S-type (middle, red), and U-type (right, blue) warped galaxies. The shaded region represents Poisson errors for each bin. For comparison, the expected isotropic distribution with the same number of central and satellite galaxies is shown as a gray horizontal line, while the 3σ range of its random distribution is shaded in gray. For S- and U-type warped galaxies, significant anisotropies appear, with satellites preferentially clustering at 45° < ϕ < 90°. Lower: same as the upper panels, but for central galaxies that host at least six satellites (Nsat ≥ 6).
Paper: Warped Disk Galaxies. II. From the Cosmic Web to the Galactic Warp
Authors: Woong-Bae G. Zee, S. Lyla Jung, Sanjaya Paudel, Suk-Jin Yoon
Figure caption: Left: number of satellites per host, Nsat, vs. distance to the nearest filament, rfila, for the unwarped control sample (black dashed). The shaded band shows the standard deviation for each bin. Middle: same as left, for S-type warped galaxies (red); the control is overplotted for comparison. Right: same as left, for U-type warped galaxies (blue); the control is overplotted.
Paper: Warped Disk Galaxies. II. From the Cosmic Web to the Galactic Warp
Authors: Woong-Bae G. Zee, S. Lyla Jung, Sanjaya Paudel, Suk-Jin Yoon
Figure caption: Left: the normalized histogram of the distance to the nearest filament, rfila, for the unwarped control sample (dashed black), S-type (red), and U-type warped galaxies (blue). Middle: fraction of warped galaxies of S-type (red) and U-type (blue) as a function of Dfila. The shaded region represents Poisson errors in each rfila bin. Right: same as the middle panel, but for strongly warped galaxies (﹩\alpha \geqslant 4\mathop{.}\limits^{^\circ }9﹩).
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: N2 BPT diagrams for our sample galaxies residing in the cores of the three protocluster fields. Stacked data are from Table 4, and individual galaxy data are from Table 3. The individual galaxy with measurements is indicated by cyan points, and blue point is the full stacked sample using 43 galaxies in the protocluster fields. The red point is the high-mass stacked sample and the purple point is the low-mass stacked sample. The grayscale histogram corresponds to the distribution of local SDSS galaxies. The blue curve is the maximum starburst model of L. J. Kewley et al. (2001). The green line and the orange line both represent observational data, with the green line coming from A. E. Shapley et al. (2015) and the orange line from C. C. Steidel et al. (2014). The weight parameter represents the fractional contribution of shocks to the combined model. Left: BPT diagrams with pure H II region photoionization model (shown in pink). Right: BPT diagrams incorporating the H II region plus shock-wave photoionization models at two different metallicities: 0.4 Z⊙ (shown in wheat) and 0.15 Z⊙ (shown in green).
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: Density maps of the three massive galaxy protoclusters at z ≈ 2.2 presented in this work. In all three panels, the gray thin contours mark galaxy overdensity (δg) in steps of 0.2 arcmin−2, with the inner density peaks reaching ∼2 arcmin−2. For the BOSS1244 and BOSS1542 protocluster fields, δg is estimated based upon the surface density of the Hα emitters (HAEs) at the protocluster redshift, identified from ground-based broad+narrow band imaging, whereas for the BOSS1441 field, δg is from the Lyα emitters (Z. Cai et al. 2017; D. D. Shi et al. 2021). The blue squares mark the locations of the HST WFC3/G141 pointings of the MAMMOTH-Grism survey (GO-16276, PI Wang, X. Wang et al. 2022b), and the red rectangles (each with a 3′ × 6′ FoV) show the masks of our Keck/MOSFIRE K-band follow-up spectroscopy (2022A_U016, 2023A_U139, PI Malkan). The general properties of our three protocluster fields are given in Table 1, and the detailed information about our Keck observations is shown in Table 2.
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: O32 vs. R23 diagram for our sample galaxies. The cyan points indicate individual high-redshift galaxies from the sample, while the blue point represents the stacked sample of all galaxies. The purple point corresponds to the stacked sample of low-mass galaxies, and the red point denotes the stacked sample of high-mass galaxies. Error bars represent uncertainties in the measurements. The gray background shows the line ratios of local galaxies from the Sloan Digital Sky Survey (SDSS) for comparison. The color bar adopts the calibration described in F. Bian et al. (2018). The pure H II region photoionization model, featuring varying ionization parameters and metallicities, is shown in pink.
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: Flux-calibrated G141 grism spectra for object gal02588, as listed in Table 3. The spectrum is from HST observations and has been processed using GRIZLI software. The 1D spectrum is displayed as a blue line, while the Gaussian fit is overplotted in red. The uncertainty is illustrated by the light blue shaded area. The bottom panel presents the corresponding 2D spectrum.
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: The mass–metallicity relation for our galaxy sample is shown, where the cyan points represent individual high-redshift galaxies, with error bars indicating 1σ uncertainties in the measurements. For comparison, the MOSDEF sample (R. L. Sanders et al. 2021) is plotted in blue, with light blue error bars denoting the uncertainties. Additionally, we include the protocluster sample from Yang et al. (2025, in preparation), marked by red dashed lines.
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: Flux-calibrated K-band spectrum for object gal02588, as listed in Table 3, observed with the Keck MOSFIRE instrument. The color-coding and styles of the symbols and lines follow exactly those shown in Figure 2. The left panel displays the covered emission lines of Hα and [N II], whereas the right panel shows [S II].
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: Stacked 1D MOSFIRE spectra for 43 galaxies at z ∼ 2.2 in three massive protocluster fields (BOSS1244, BOSS1441, and BOSS1542). In the spectral plot, the blue curve shows the bootstrapped spectrum, the cyan bands indicate the bootstrapped flux uncertainties, and the red dashed curves show the best-fit Gaussian fits to multiple emission lines (Hα, [N II], [O I], [S II]). The details of the stacking procedures are provided in Section 4.2.
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: S2 BPT diagrams for local and our sample galaxies residing in the cores of the three protocluster fields. The color-coding and styles of the symbols and lines follow exactly those shown in Figure 7.
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: O1 BPT diagrams for local and our sample galaxies residing in the cores of the three protocluster fields. The color-coding and styles of the symbols and lines follow exactly those shown in Figure 7.
Paper: MAMMOTH-MOSFIRE: Environmental Effects on Galaxy Interstellar Medium at z ∼ 2
Authors: Hang Zhou, Xin Wang, Matthew A. Malkan, Tommaso Treu, Yiming Yang, Zheng Cai, Xiaohui Fan, Mengting Ju, Dong Dong Shi, Anahita Alavi, Fuyan Bian, James Colbert, Alaina L. Henry, Sijia Li, Zihao Li, Harry I. Teplitz, Hu Zhan, Xian Zhong Zheng, Zheng Zheng, Yifei Jin
Figure caption: The velocity dispersion vs. log([O I]/Hα) diagnostic diagram for our sample galaxies. The cyan data points represent our sample of protocluster galaxies. The solid lines show theoretical model grids from MAPPINGS V for two metallicities: 0.15 Z⊙ (left panel, red) and 0.4 Z⊙ (right panel, blue). Within each grid, the sequence of models represents different mixing fractions between a pure H II region model and a pure shock model. The intermediate lines indicate different shock contributions, ranging from 0% to 100%, as indicated by the black labels.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: The FWHM is a function of MWD. The 127 novae follow a highly significant trend. The green curve is for 0.23 times the escape velocity of the WD. Through most of the range, it is adequate to quantify the model as ﹩1{0}^{({M}_{{\rm{WD}}}/2)}﹩ × 500 km s−1. The escape velocity has an increasing deviation as the Chandrasekhar mass is approached, with this being seen both in the escape-velocity model and in the nova data. Indeed, for masses >1.3 M⊙, the observed upward deviations are substantially larger than predicted by the escape velocity alone. The scatter is large, but is consistent with the ±0.15 M⊙ for the real uncertainty in the masses and with the ±0.22 for the real uncertainty in the logarithm of FWHM. Two typical error bars are presented for two of the points. That is, the observations look to closely follow a single function, while the known measurement uncertainties produce the observed scatter in the plot. With this, the real intrinsic relation is consistent with Equation (4) with no variation.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: The differences in MWD between the original Shara masses and masses from other sources. This is a comparison test, where the original Shara masses vary systematically with MWD, following a linear trend (the green line). The original Shara masses are systematically too large for low-mass novae. This is true for the three independent sets of WD masses, from the RV measures in the H. Ritter & U. Kolb (2003) catalog, the model WD masses from Hachisu–Kato (H&K), and the mixture of methods collected as “other.” The significant trend is the same for the three independent data sets, proving that the original Shara masses have a systematic bias. This bias can be corrected with Equation (1).
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Shara method for measuring WD mass, with contours corrected for bias. The method of M. M. Shara et al. (2018) is to theoretically model nova light curves as a function of the WD mass (MWD) and the accretion rate, then calculating the decline rate (t2), and the nova amplitude in the V band (A). For any choice of t2 and A, a unique mass is returned. The figure plot the position of each of 80 nova analyzed in the Shara paper, with each point having a calculated mass. I have drawn contours of equal-mass as a family of green curves, one curve for each labeled mass. So for other novae not in the original Shara sample, a user need only plot the nova based on the observed t2 and A, then read off MWD from the contour lines. This allows for the extension of the Shara model calculations to many additional novae. A bias has been found for the smaller Shara masses, with this corrected by Equation (1), as represented by the contours in this plot.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Histograms for the Vpeak and D distributions. The two panels show the distributions for the 28 γ-nova (in blue) and the 95 non-γ novae from 2010.0 to 2022.6. The top panel shows the distribution of the nova peak magnitude. We see that both distributions have sharp changes at V = 8.0. Almost all novae brighter than 8 mag are detected by Fermi, while most nova fainter than 8 mag are not detected. That is, optically bright novae are usually detected by Fermi. The bottom panel shows the distribution of the nova distances, D. We see a threshold at 3500 pc, where nearer novae are usually discovered by Fermi, and farther novae are usually not detected. The primary exception for this is that a modest fraction of the novae in the Galactic bulge (with D ∼ 8000 pc) are detected. But all these bulge detections are for the fastest novae (with t3 ≤ 30 days), for which the Lγ are the brightest. This demonstrates that the visibility of novae by Fermi is controlled by both D and t3 (see Figure 10 and Equation (6)).
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Decline rate vs. WD mass. From Table 1, the decline rate (t3) is plotted vs. MWD for 74 JDF novae (red diamonds) and for 117 SPOC novae (blue diamonds). We see a highly significant straight line, on this log-linear plot, with the best fit shown with the green line, with t3 equaling ﹩1{0}^{(-1.73{M}_{{\rm{WD}}})}﹩ × 1900 days. The typical measurement errors (±0.15 M⊙ in mass and ±40% in t3) are displayed for two points. The plot has substantial scatter about the green line, but all the scatter is consistent with ordinary measurement errors, so the real underlying relation apparently has only small intrinsic scatter.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: The distance and orbital period distribution for novae with shells and without shells. E. Santamaría et al. (2025) have already proven that distant novae rarely have visible shells, due to extinction and small unresolved sizes. From this figure, the effective cutoff is something like 4000 pc. Further, from Figure 6, shell-novae have a strong bias to have orbital periods shorter than one-third of a day. These two visibility criteria make for a rectangular area in the lower left of the plot, which encloses the strong cluster of shell-novae. That is, with only four exceptions (including the famous GK Per), all the shell-novae are in the relatively small area. This is highly significant, but I do not understand why the shells are bright for P < 0.33 day.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Histogram for shell-novae and P. The overall period distribution of novae is shown by the black histogram, with the base figure taken from Figure 2 of B. E. Schaefer (2022a). The distribution of the 37 novae with both shells and P measures is overplotted as a red-shaded histogram. We see that shell-novae are strongly biased against periods longer than one-third of a day. Normal novae have 13% with red giant companions, whereas shell-novae have 0% with red giant companions. The strong bias for bright-shells from short-orbits is apparent for novae with red giant companions, subgiant companions, and main-sequence companions, so the bias does not arise from any feature of the evolutionary state of the companion (say, from a stellar wind, or surface temperature). But I do not know any mechanism for how the shell brightness depends on the companion radius or the small semimajor axis.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Histogram of WD masses for SPOC and JDF light-curve groups. The JDF light-curve classes (the red-shaded histogram) have a distinctly low-mass distribution, with an average of 0.81 M⊙ and a 1σ range extending up to 0.95 M⊙. The SPOC light-curve classes (the blue shaded histogram) have a distinctly high-mass distribution, with an average of 1.10 M⊙ and a 1σ range extending down to 0.95 M⊙. The distribution is like that expected for a sharp cutoff at 0.97 M⊙, where the known measurement errors of ±0.15 M⊙ create smearing that mixes up the two distributions around the cutoff.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Gamma-ray luminosity vs. t3. For the 25 γ-ray novae with measured decline rate t3 (see Table 4), the gamma-ray luminosity is correlated with the t3. Typical measurement error bars are shown for two novae. The scatter about the best-fit power law (the green straight line) is large. The relation is significant at the 4.2σ confidence level. This correlation is quantified with Equation (5). So, for some unknown reason, the γ-bright novae are the fast novae, with relatively high MWD.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Detectability of γ-ray novae by Fermi. In this plot of t3 vs. D, the 28 γ-novae are represented by the large blue circles, while the nondetections (from 2010.0 to 2022.6) are represented by the small red × symbols. The visibility of novae depends on the gamma-ray flux, which is Lγ/(4πD2), for which t3 is a proxy for the luminosity through Equation (5). The Fermi threshold for >100 MeV flux from a nova is observed to vary between 0.8 and 5.0 (in units of 10−7 photons cm−2 s−1). These limits are represented by the two parallel lines of constant flux, Fγ, connecting from the middle of the top down to the middle of the right side. The unshaded-region below the bottom line is for novae that are above the highest of the detection thresholds, and the darkly shaded region to the upper right of the upper line is for bursts that are fainter than the lowest thresholds. The middle lightly shaded region is for the variable detection threshold of Fermi, where some novae will be detected, and some novae will be missed. This figure presents the explanation for why Fermi only discovers 20% of novae. Further, this figure demonstrates that γ-novae are not a separate class of novae; rather, they are just the novae that are near enough to be detected.
Paper: Comprehensive Listing of 208 Nova White Dwarf Masses as the Primary Determinant of Spectral Class and Light-curve Class
Authors: Bradley E. Schaefer
Figure caption: Table 1 contains the primary data product of this paper, with the comprehensive catalog of nova properties (including MWD and Vq) for all 402 Galactic novae, while this figure summarizes the science results from this paper. This figure works with a vertical line intersecting the various number lines to show a possible or likely property for any single nova. For example, a vertical line that crosses the bottom number line at 0.7 M⊙ points to a nova with an FWHM of 1100 km s−1, t3 near 120 days, a light-curve shape from the J, D, or F classes, an Fe II spectral class, possibly a neon nova, and certainly not a recurrent nova. A known RN will have a mass 1.2–1.4 M⊙, FWHM 2000–6000 km s−1, t3 6–18 days, a light-curve shape from the S, P, O, or C classes, a He/N spectral class, and possibly be a neon nova. The t3 number line is related to the WD mass by Equation (2), the FWHM is from Equation (4), the division between JDF and SPOC classes is near 0.95 M⊙, and the division between Fe II and He/N spectral classes is near 1.15 M⊙. These divisions and equations are consistent with being exact relations with substantial superposed measurement errors. Nevertheless, there could easily be real scatter and outliers to some modest degree.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: MAVEN crossing of the Martian induced magnetosphere on 2014 December 29. The time series of the magnetic field in MSO coordinates, the energy–time spectrogram of ions, electrons, and solar wind ions. The crossings of the bow shock and the tail CS are labeled by vertical black and red dashed lines, respectively.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: Diagram illustrating the method used to estimate the shift of the CS. The unshifted CS is shown as a thick black line, while the CS crossing observed by MAVEN is marked as point P. Thin dashed black lines represent possible configurations of a displaced CS, with corresponding crossing points labeled as ﹩P^{\prime} ﹩. The CS normal vector, denoted as ﹩\hat{n}﹩, consistently points from the +BX hemisphere to the −BX hemisphere. The deviation angle α, defined between vector ﹩{{\boldsymbol{O}}{\boldsymbol{P}}}^{{\rm{{\prime} }}}﹩ and ﹩\hat{n}﹩, exceeds 90° when the CS is significantly displaced toward the +BX hemisphere and is less than 90° when displaced toward the −BX hemisphere. Figure adapted from Z. Rong et al. (2016) and G. A. DiBraccio et al. (2017).