adsabs/AstroCLIMB huggingface dataset:
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: The corner plot of the average selection function of the models, with Λ = 16 for the blue arm. Those for the red arm are similar, so we do not show them in a separate figure. The diagonal panels show marginalized TPR (detectability) for the blue/red arm in blue/red and the relative distribution of the training set in gray.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: Color-coded spectra against folded phase derived from Kepler light curves for KIC 5444392 (top panel) and KIC 6526196 (bottom panel). The spectra with ﹩{p}_{50}^{{\rm{\Lambda }}=16}\gt 0.5﹩ are shown using the “jet” color map, while others are shown using the “gray” color map. For briefness, only Mg b and Hα regions are shown.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: Selected spectra of KEBC objects, including 1392 blue arm and 1492 red arm spectra. Color codes the periods. The thick gray lines represent the fraction of spectra with ﹩{p}_{50}^{{\rm{\Lambda }}=16}\lt 0.5﹩. 0 and 1 are the phases corresponding to major eclipses.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: The distribution of binary probabilities of the SB2s in APOGEE DR16&17 (Kounkel et al. 2021) observed by LAMOST MRS. The left/right panels show blue/red arms. Top panels are for the very short period SB2s (P < 10 days), while bottom panels are for SB2s with P > 10 days.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: The distribution of ﹩{p}_{q}^{{\rm{\Lambda }}}﹩ for the 5 million LAMOST MRS DR8 spectra with S/N > 5, normalized for each S/N bin. Both high Λ and high q values suppress false positives.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: This figure demonstrates how binary spectra are synthesized in our experiment. The top and bottom panels show the relative flux and normalized flux, respectively. The initial mass of the primary star is 1 M ⊙, and that of the secondary is 0.9 M ⊙ (q = 0.9). Both of them have solar metallicity and an age of 5 Gyr. A 100 km s−1 RV separation is applied. Differences could be found by comparing the spectra of the primary star and the binary, which indicates that a classification is possible to some extent.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: The stellar parameters of 1000 randomly chosen mock binaries in our training set. The left and right panels show primary stars and secondary stars, respectively. Color codes the luminosity ratios. Superposed are a set of isochrones with solar metallicity but different ages.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: The average FPRs and TPRs against Λ.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: Each panel in this figure shows the performance of our CNN models on mock MS A-, F-, G-, K-, and M-type twin binaries (q = 1) at different S/N and ﹩{v}_{\mathrm{eq}}\sin i﹩ values, assuming that the two components in the binary system share the same parameters T eff, ﹩\mathrm{log}g﹩, [Fe/H], [α/Fe], and ﹩{v}_{\mathrm{eq}}\sin i﹩.
Paper: The Spectroscopic Binaries from the LAMOST Medium-resolution Survey. I. Searching for Double-lined Spectroscopic Binaries with a Convolutional Neural Network
Authors: Bo Zhang, Ying-Jie Jing, Fan Yang, Jun-Chen Wan, Xin Ji, Jian-Ning Fu, Chao Liu, Xiao-Bin Zhang, Feng Luo, Hao Tian, Yu-Tao Zhou, Jia-Xin Wang, Yan-Jun Guo, Weikai Zong, Jian-Ping Xiong, Jiao Li
Figure caption: The architectures of our CNN models for blue and red arms.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: The baseline-divided spectrum extracted on-source (orange) compared with the outflow spectrum extracted at (−1″, −1″) from the submillimeter continuum peak (blue). Both spectra are extracted with a fixed 1″ aperture. The on-source spectrum is multiplied by −1 for better visual comparison with the outflow spectrum. The weaker emission lines at 5–7 μm in the on-source spectrum are mostly H2O and CO discussed in Section 4, and the noise in the ∼9–11 μm range of both spectra is due to the fringe residual. The continuum is derived by convolving a Gaussian profile with a width of 10 channels. Imperfect continuum subtraction appears around major ice features, such as ∼7 and ∼15 μm. Identified emission lines are annotated.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: MIRI images with F560W, F770W, and F1000W filters taken in parallel with the background pointing. The identified four shell-like structures are highlights in the panel of the F560W image (left). The image on the right shows the archival Spitzer IRAC 3 image taken on 2004 September 3, where the MIRI F560W image convolved with the IRAC 3 resolution of 1.″88 is shown in logarithmic contours from 1 to 150 MJy sr−1. The field of view of the MIRI imager leaves a distinct shape at the top left of the images. The red cross labels the submillimeter continuum peak position.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Ice features in the 11–12 μm region of the spectrum. Left: the MRS spectrum and the continuum fit. The continuum is fitted locally with a fifth-order polynomial using ±0.01 μm regions around 10.18–10.22 μm, 10.38–10.42 μm, 10.58–10.62 μm, 11.78–11.82 μm, 12.18–12.22 μm, 12.38–12.42 μm, and 12.48–12.52 μm as anchor points (gray hatched regions). Right: the optical depth spectra compared to laboratory spectra of C2H5OH, CH3CHO, and HCOOCH3. The crosshatched region highlights the overlapping range of two subbands, which has a less stable baseline.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Continuum-subtracted intensity maps of [Fe II] lines at 25.988 and 17.935 μm, [S I] at 25.249 μm, [Ne II] at 12.814 μm, H2 S(5) and S (7) at 6.910 and 5.511 μm, respectively. The map is calculated from the average intensity within ±200  km s−1 from the rest-frame line centroids. The continuum is calculated from −500 to −300  km s−1. The red cross labels the submillimeter continuum peak position. The dotted circles indicate the extraction aperture for the spectrum shown in Figure 10.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Continuum-subtracted spectra showing emission from the CO fundamental P-branch and the H2O bending mode centered on 6 μm. The data, which are shown with an offset of 0.3 mJy, are modeled by a simple slab model for line identification (Salyk et al. 2011; Salyk 2020). Emission lines other than H2O and CO are annotated.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Ice features in the 8–11 μm region of the spectrum. Left: the MRS spectrum and the continuum fit. The continuum is fitted locally with a fourth-order polynomial using 8.18–8.22 μm, 8.48–8.52 μm, 10.18–10.22 μm, and 10.48–10.52 μm as anchor points (gray hatched regions). Right: the optical depth spectrum labeled with potential carriers. The red shaded region highlights the range of the NH3 umbrella mode in various ice mixtures investigated in Bottinelli et al. (2010).
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Ice features in the spectra from 7 to 8 μm. Left: the MRS spectra and the fitted continuum. The continuum is fitted locally with a third-order polynomial anchored at 6.99–7.01 μm, 7.12–7.14 μm, 7.94–7.96 μm, and 7.99–8.01 μm (gray hatched regions). Right: the optical depth spectra labeled with potential carriers.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Optical depth spectra compared with a composite spectra of several ice species measured from experiments. The details of the laboratory data are discussed in Appendix C. The “CO2” spectra (red) are from pure CO2.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Spectra of the CO2 ice feature at 15.2 μm. The MIRI spectra zoomed to the CO2 ice features are shown in the left panel. A local baseline (orange) is fitted with a third-order polynomial using the spectra in 14.5–14.7 μm and 16.3–16.5 μm. The derived optical depth spectra are shown in the right panel.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Left: the MIRI MRS spectra compared with Spitzer/IRAC aperture photometry (black). Both data were extracted with a 3″ aperture. The red square shows the MRS spectra convolved with the IRAC 4 filter. The error bars indicate an assumed 10% uncertainty. The aperture photometry is aperture corrected but without color corrections. Right: the MRS 1D spectra along with the scaled Spitzer/IRS spectra at long wavelengths. The scaling factor increases linearly with wavelength to match the wavelength dependency in the extraction aperture of the MRS 1D spectra.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Top: the 1D spectra extracted with aperture sizes of two, four, six, and eight beams without scaling. Bottom: the 1D spectra extracted with a four-beam aperture with and without scaling.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Selected absorption features detected in the MIRI MRS spectra compared with archival Spitzer/IRS spectra.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Top: extracted MIRI MRS spectrum of the IRAS 15398−3359 point source, with major solid-state features indicated. The wavelength axis is in logarithmic scale. The dashed line illustrates the fitted continuum. Top (inset): detail of the 5.5–8 μm region from the same spectrum with secure and possible identifications labeled (see Table 1). Bottom: the optical depth spectrum derived using the continuum shown in the top panel.
Paper: CORINOS. I. JWST/MIRI Spectroscopy and Imaging of a Class 0 Protostar IRAS 15398–3359
Authors: Yao-Lun Yang, Joel D. Green, Klaus M. Pontoppidan, Jennifer B. Bergner, L. Ilsedore Cleeves, Neal J. Evans II, Robin T. Garrod, Miwha Jin, Chul Hwan Kim, Jaeyeong Kim, Jeong-Eun Lee, Nami Sakai, Christopher N. Shingledecker, Brielle Shope, John J. Tobin, Ewine F. van Dishoeck
Figure caption: Left: the MIRI MRS spectrum of IRAS 15398−3359 along with a second-order polynomial baseline fitted at 6.59–6.61 μm and 6.79–6.81 μm (gray hatched regions). Right: the optical depth spectra of the shallow absorption at 6.68–6.72 μm. The purple shaded region shows the scaled laboratory absorbance spectrum from Gerakines et al. (1996). The narrow emission features are predominantly due to warm gas-phase water (Section 4).
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: The marginal posterior distributions for the maximum mass of field BBHs (left) and the difference between the mean values of spin magnitudes for the stellar-originated BHs and dynamical 2G BHs (right).
Paper: Satellite Constellation Avoidance with the Rubin Observatory Legacy Survey of Space and Time
Authors: Jinghan Alina Hu, Meredith L. Rawls, Peter Yoachim, Željko Ivezić
Figure caption: Satellite avoidance maps constructed for the Rubin scheduler for each simulated constellation. Each is for a twilight observation period of 90 minutes (beginning after sunset with a Sun altitude of −17.°1). The map projections are rotated so zenith is in the center of the image. Darker regions have more illuminated satellites and therefore more negative weighting. By varying the dodging weight placed on these maps, the scheduler will more actively avoid regions of the sky where satellites could streak images.
Paper: Satellite Constellation Avoidance with the Rubin Observatory Legacy Survey of Space and Time
Authors: Jinghan Alina Hu, Meredith L. Rawls, Peter Yoachim, Željko Ivezić
Figure caption: Three simulated satellite constellations, one per column. Starlink Gen1 is 4408 satellites, Starlink Gen2 is 29,988 satellites, and OneWeb is 6372 satellites, for a grand total of 40,768. The top row shows the 3D distribution of each constellation around Earth. The middle row shows an instantaneous Hammer projection of the altitude and azimuth positions of each constellation as seen from Rubin Observatory on 2023 October 1, during twilight (Sun altitude −18°). Blue points are satellites illuminated by the Sun at this time, red points are satellites not illuminated by the Sun, and black points are satellites that are both illuminated and above the Rubin 20° altitude pointing limit. The bottom row is the same Hammer projections 6 hr later in the middle of the night (Sun altitude −50°). Because Starlink satellites orbit at 550 km, none are illuminated in the middle of the night at this time of year. The OneWeb constellation at 1200 km has only a single illuminated satellite above the Rubin altitude limit at this particular time.
Paper: Satellite Constellation Avoidance with the Rubin Observatory Legacy Survey of Space and Time
Authors: Jinghan Alina Hu, Meredith L. Rawls, Peter Yoachim, Željko Ivezić
Figure caption: Illustration of changes in the mean streak length in all visits including those with no streak (top left), the fraction of visits with streaks (top right), the number of acquired visits in year 1 (bottom left), and coadded depth in the g band (bottom right) as a function of dodging basis function weight (starting with essentially no dodging on the left). Note that to reduce the fraction of visits with streaks by about a factor of 2, satellite avoidance will require 10% of total observing time.
Paper: Satellite Constellation Avoidance with the Rubin Observatory Legacy Survey of Space and Time
Authors: Jinghan Alina Hu, Meredith L. Rawls, Peter Yoachim, Željko Ivezić
Figure caption: Impacts of satellite streaks on simulated LSST observations without any satellite avoidance. Compared to standard LSST observations (top), twilight NEO observations (bottom) cannot easily be shifted to avoid satellites. The left panels show the altitude and azimuth distribution of observations on the sky (zenith at the center of the plots), and the right panels show how many streaks would result from the three simulated satellite constellations as a function of how high above the horizon the telescope is pointing (observation altitude). Note that most twilight NEO observations would contain a satellite streak.
Paper: Satellite Constellation Avoidance with the Rubin Observatory Legacy Survey of Space and Time
Authors: Jinghan Alina Hu, Meredith L. Rawls, Peter Yoachim, Željko Ivezić
Figure caption: The trade-off between the mean streak length and final median coadded depth in the g band for one year of the LSST (controlled by dodging basis function weight). A negative change in coadded depth indicates the survey is shallower.
Paper: Erratum: “Near-infrared Accretion Signatures from the Circumbinary Planetary-mass Companion Delorme 1 (AB)b” (2022, ApJL, 935, L18)
Authors: S. K. Betti, K. B. Follette, K. Ward-Duong, Y. Aoyama, G.-D. Marleau, J. Bary, C. Robinson, M. Janson, W. Balmer, G. Chauvin, P. Palma-Bifani
Figure caption: Predicted line ratios for local line excitation (“stellar”; Kwan & Fischer 2011, blue squares), and accretion shock emission (“planetary”; Aoyama et al. 2018, purple/yellow circles) models. Delorme 1 (AB)b’s NIR line ratios (panels (a)–(c)) are shown in black with markers (stars, diamonds) with updated line flux uncertainties. Panel (d) shows Paγ/Hα line ratios with updated NIR uncertainties, with Delorme 1 (AB)b values (unfilled markers) derived from our Paγ observations and the noncontemporaneous Hα measurement of Eriksson et al. (2020).
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: Posterior distribution the parameters about the dynamical channel for the OnePL and the TwoPL models; note that r 2G is the fraction of 2G BHs in the dynamical environment, and f 2G is the fraction of BBHs involving a least one 2G BH.
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: Posterior predicted check for the reconstructed primary mass distribution (top left), the mass ratio distribution (top right), the effective inspiral spin distribution (bottom left), and the effective precessing spin distribution (bottom right).
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: The reconstructed astrophysical distributions for the cosine of the spin-tilted angle (left) and the spin magnitude (right). The shaded areas indicate the 90% credible regions.
Paper: Potential Subpopulations and Assembling Tendency of the Merging Black Holes
Authors: Yuan-Zhu Wang, Yin-Jie Li, Jorick S. Vink, Yi-Zhong Fan, Shao-Peng Tang, Ying Qin, Da-Ming Wei
Figure caption: The same as Figure 2, but for the PPISN Peak model.