adsabs/AstroCLIMB huggingface dataset:
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Comparison of measured and simulated absorbances of C2H6 (top) and C2H2 (bottom) for a spectral resolution of 0.45 cm−1 in the case of the H2:CH4:N2 gas mixture after 24 hr of irradiation at 473 K. The simulated spectra were obtained following the procedure described in Section 2.2.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Evolution of the methane consumption efficiency (﹩{{\boldsymbol{e}}}_{{\mathrm{CH}}_{4}})﹩ as a function of time of irradiation obtained with a 0D thermo-photochemical model. Simulations were made for an H2:CH4:N2 (99%:0.5%:0.5%) initial gas mixture, a pressure of 15 mbar, and different gas temperatures: 295, 473, 673, 873, and 1073 K. ﹩{e}_{{\mathrm{CH}}_{4}}﹩ at 105 s are presented as function of the temperature in Figure 13(a).
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Comparison of measured and simulated absorbances of CO for a spectral resolution of 0.45 cm−1 in the case of the H2:CH4:N2 gas mixture after 24 hr of irradiation at 295 K. The simulated spectrum was obtained following the procedure described in Section 2.2. Residual (measured – simulated) is shifted vertically for clarity.
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Temperature measured in Fleury et al. (2019) at different positions of the quartz tube for different set oven temperatures: 573, 873, and 1173 K. Temperature profiles were obtained using Equation (1). 0 cm corresponds to the center of the cell, where the temperature is maximal (T max).
Paper: Experimental Investigation of the Photochemical Production of Hydrocarbons in Warm Gas Giant Exoplanet Atmospheres
Authors: Benjamin Fleury, Yves Benilan, Olivia Venot, Bryana L. Henderson, Mark Swain, Murthy S. Gudipati
Figure caption: Comparison of measured and simulated absorbances of CH4 for a spectral resolution of 0.45 cm−1 in the case of the H2:CH4:N2 gas mixture after 22 hr at 673 K. The simulated spectrum was obtained following the procedure described in Section 2.2. Residual (measured – simulated) is shifted vertically for clarity.
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: (a) and (b) The comparison between model calculations and experimental measurements for proton and helium spectra. Here the red shadowed shape represents the contribution of local SNR (e.g., Geminga), the blue solid line the background components, and the black solid line the total contribution. The data points are measured by AMS-02, CREAM, DAMPE, and CALET experiments (Aguilar et al. 2015a, 2017; Yoon et al. 2017; An et al. 2019; Alemanno et al. 2021; Adriani et al. 2022a; Brogi et al. 2022).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Similar to Figure 2, the individual species of C, O, Ne, Mg, Si, and Fe are shown in panels (a)–(f). The data points are from the AMS-02 and CALET experiments (Aguilar et al. 2017; Adriani et al. 2020; Aguilar et al. 2020, 2021b; Adriani et al. 2021).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Cartoon illustration describing the production mechanism of the multi-messenger anomalies: the spectral hardening and break-off at a rigidity of 200 GeV and 5 TeV for both primary and secondary nuclei, the energy cutoff for the secondary positrons and electrons at around 300 GeV and 1 TeV, respectively.
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: The observed and calculated all-particle spectra. In the model calculations, the solid blue, orange, green, red, and black lines represent the P + He, C + N + O, Ne + Mg + Si, Fe species, and all-particle spectra respectively. The data points are measured by the TALE (Abbasi et al. 2018), Tibet-ASγ (Amenomori et al. 2008), and IceTop (Aartsen et al. 2019, 2020) experiments, and weighted by Hörandel (Hörandel 2003).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: (a)–(c) Similar to Figure 2, the individual species of N, Na, and Al, including both primary and secondary components. The data points are from the AMS-02 experiment (Aguilar et al. 2018a, 2021c).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Comparison between model calculations and observations for the ratios of primary to primary species. The red solid lines with the shadows indicate the contributions from the nearby SNR. The black solid lines represent the ratio results of the model expectation taking into account the nearby source component. The data points are adopted from AMS-02 measurements (Aguilar et al. 2017, 2018a; Adriani et al. 2020; Aguilar et al. 2020, 2021c, 2021b).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Comparison between model calculations and observations for the ratios of secondary to primary species. The data points are adopted from AMS-02, CALET, and DAMPE measurements (Aguilar et al. 2016a, 2016b, 2018b; Adriani et al. 2022b; DAMPE Collaboration 2022).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Similar to Figure 2, the spectra of positrons and electrons, their sum from panels (a)–(c), and the ratio of positron to the sum of positrons and electrons in panel (d). The data points are adopted from the AMS-02 and CALET experiments (Adriani et al. 2017, 2018; Aguilar et al. 2019a, 2019b).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Comparison between model calculations and the upper limit of the amplitude and phase of anisotropy for CREs. The data points are adopted from Abdollahi et al. (2017).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: (a)–(d) Similar to Figure 2, the secondary particles of ﹩\bar{p},\mathrm{Li},\mathrm{Be}﹩, and B. The data points are from the AMS-02 and CALET experiments (Aguilar et al. 2016a, 2018b; Adriani et al. 2022b).
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Similar to Figure 8. Comparison between model calculations and observations for the ratios of secondary to secondary species. The data points are adopted from AMS-02 measurements (Aguilar et al. 2016a, 2018b).
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: HST F160W imaging spatial decomposition with GALFIT. (a) Imaging data. (b) Model (3), where the legend gives the two quasar point sources and lens galaxy Sérsic profile. (c) The image with only the point sources subtracted, leaving residuals due to the lensing galaxy but also the strong contribution from the S host galaxy. (d) The full model subtracted from the data, where the residuals are scaled by σ significance above the remaining background. While the PSF models leave residuals corresponding to the host galaxies, the central lensing galaxy is well constrained. (e) Radial profile starting from the center of the N PSF. The lower subpanel shows the scaled residuals as a function of radius. Model (3) does a reasonably good job out to a radius of ∼1″, beyond which the brightness from the extended host galaxies falls off rapidly. The S host component closely follows the S PSF component, while the N host component is heavily suppressed. Major tick marks in panels (a)–(d) are 0.″5.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Observed-frame optical spectra for the two quasars. Top: we show the HST/STIS spectra for SDSS J0823+2418 as well as the Gemini/GMOS spectra, indicated by the legend. The STIS spectra have been smoothed with a Gaussian kernel with σ = 1 for readability. Green shaded regions are heavily affected in the GMOS spectra by telluric absorption. Bottom: flux ratios between the N and S quasars for the STIS and GMOS spectra. Dashed lines show the average of the corresponding flux ratio, with values that are roughly consistent with those found with photometry. The N and S spectra from both instruments are quite similar, suggestive that the system is a single lensed quasar where the N source is more magnified than the S component.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Same as Figure 5, but for Keck AO imaging. We again show model (3). The extended host components appear more prominent in the K p band, but do not contribute much to the radial profile beyond a radius of 1″. The irregular shape of the PSF is due to the adaptive optics of Keck. Major tick marks in all panels are 0.″25. In panel (c), the faint blob above the S PSF could be a faint foreground galaxy. There also appears to be an arc to the residual structure of the N galaxy that is mirrored in the S galaxy. This overall ellipsoid arrangement suggests some degree of lensing shear.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Spectral fitting of the HST/STIS spectra for SDSS J0823+2418. The top and bottom sets of panels show the fits for the N and S targets, respectively. The spectra are fit with a pseudo-continuum model composed of a power law combined with a low-order polynomial (orange curve) and the Fe II template. Gray regions are masked out during the fit due to lingering cosmic rays. The lower inset panels show zoom-ins on the local fits of broad emission lines after continuum subtraction.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Same as Figure 7, but spectral fitting of the Gemini/GMOS spectra. Gray regions are masked out primarily to avoid regions that are heavily affected by telluric absorption bands. The extended range toward bluer wavelengths allows for a better fit of the C III] emission line than is possible with the STIS spectra.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: HST/WFC3 color composite image from Paper I, where F475W is coded in blue, F814W in red, and the average of F475W and F814W bands in green. The Gaia DR2 source positions are marked by the green crosses. The angular and physical separations between the double sources are given in the bottom right corner.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: GMOS spectral extraction. Top: 2D spectrum with the extraction regions marked in white. We highlight the position of the bright Mg II emission line. Bottom: collapsed 1D profiles and corresponding extraction regions.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: STIS spectral extraction. Top: 2D spectrum with the extraction regions marked in white. We highlight the position of the bright Mg II emission line. Bottom: collapsed 1D profiles and corresponding extraction regions.
Paper: Nearby SNR: A Possible Common Origin of Multi-messenger Anomalies in the Spectra, Ratios, and Anisotropy of Cosmic Rays
Authors: Bing-Qiang Qiao, Yi-Qing Guo, Wei Liu, Xiao-Jun Bi
Figure caption: Comparison between model calculations and observations of the amplitude and phase of anisotropy for CRs. The data points are taken from underground muon detectors: Norikura (Sakakibara et al. 1973), Ottawa (Bercovitch & Agrawal 1981), London (Thambyahpillai 1983), Bolivia (Swinson & Nagashima 1985), Budapest (Swinson & Nagashima 1985), Hobart (Swinson & Nagashima 1985), London (Swinson & Nagashima 1985), Misato (Swinson & Nagashima 1985), Socorro (Swinson & Nagashima 1985), Yakutsk (Swinson & Nagashima 1985), Banksan (Andreyev et al. 1987), Hong Kong (Lee & Ng 1987), Sakashita (Ueno et al. 1990), Utah (Cutler & Groom 1991), Liapootah (Munakata et al. 1995), Matsushiro (Mori et al. 1995), Poatina (Fenton et al. 1995), Kamiokande (Munakata et al. 1997), Marco (Ambrosio et al. 2003), and SuperKamiokande (Guillian et al. 2007); and air shower array experiments: PeakMusala (Gombosi et al. 1975), Baksan (Alexeyenko et al. 1981), Norikura (Nagashima et al. 1989), EAS-TOP (Aglietta et al. 1995, 1996, 2009), Baksan (Alekseenko et al. 2009), Milagro (Abdo et al. 2009), IceCube (Abbasi et al. 2010, 2012), IceTop (Aartsen et al. 2013), ARGO-YBJ (Bartoli et al. 2015), Tibet (Amenomori et al. 2005, 2015, 2017), and K-Grande (Chiavassa et al. 2015).
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Top row: VLA Ku-band image decomposition of SDSS J0823+2418 at 15 GHz. We show from left to right: the continuum image, the model using imfit, and the residual map. The restoring beam is shown in gray in the bottom right corner of each panel. Contours begin at 3 times the rms background and increase exponentially to the peak value. The legend in the right panel indicates the N and S radio components, as well as the compact central blob that might correspond to the foreground lensing galaxy. We overlay the HST F160W best-fit coordinates, aligned by the N source, which show agreement to within 0.″1. Major tick marks are spaced by 0.″5. Bottom row: same as the top row, but for the VLA C-band continuum imaging at 6 GHz. The best-fit locations between the two bands are consistent to within 0.″1. While the N source is clearly brighter and more spatially extended at 6 GHz, the reverse situation is seen in the 15 GHz image, indicating different spectral slopes between the N and S quasars. We do not find evidence for a lensing galaxy component in the 6 GHz frame.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Chandra X-ray observations and image decomposition. Top row: imaging of observations (1) and (2) (left and right panels) for SDSS J0823+2418 where the color bar indicates observed broadband counts. In observation (1), no source is detected for the S quasar. In observation (2), we mark the best-fit locations of the two sources from BAYMAX. The location of the brightest pixels has shifted noticeably between the two observations. Bottom left: BAYMAX assessment of joint posterior distribution for separation and flux ratio of two sources, which is roughly consistent with our GALFIT modeling results. Bottom right: decomposition of the broadband counts for observation (2), assigning each count to the most likely source.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: SEDs for SDSS J0823+2418. The top and bottom panels show the SEDs for the N and S source, respectively. We also plot optically luminous (OL), optically dim (OD), and the mean (All) SEDs of optically selected quasars from SDSS as a comparison (Richards et al. 2006a). Typical SEDs of optically bright nonblazar radio-loud (RL) and radio-quiet (RQ) quasars are also plotted for reference (Shang et al. 2011). The literature SEDs are normalized to the HST F814W luminosities of the target. For the N source, we plot the X-ray luminosity from observation (1) using a colorless star. The pink stars refer to observation (2) luminosities in both panels. For the F160W fluxes, the red squares refer to model (3), while the colorless squares refer to model (1) (N value is nearly identical in both models).
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Lens mass modeling for SDSS J0823+2418. The columns give the decompositions for the HST F160W fitted results based on model (1) (left) and model (3) (right). Top: image plane, where red triangles denote the observed relative positions of the N and S sources, the central blue dot is the location of the lensing galaxy as determined from our GALFIT analysis, and the blue ellipse is the critical curve. Bottom: decomposed source plane using glafic (Oguri 2010), where the red triangle shows the position of the single quasar relative to the cut and caustic. Despite the differing parameter values derived by GALFIT, both models can be well-described by strong lensing using a simple single isothermal ellipsoid (SIE) model.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Chandra X-ray spectral fitting for SDSS J0823+2418 using BAYMAX. The target is denoted as either north (N) or south (S) in the label, and observation number is given in parentheses. The S nucleus is not detected in the first observation, and then dominates in the later observation. The spectral shapes are fairly similar. Although the N source appears to have a less steep cutoff in the soft X-ray regime than the S source for both observations, this is likely due to the lowest-energy data point, which has a large uncertainty.
Paper: Varstrometry for Off-nucleus and Dual Subkiloparsec Active Galactic Nuclei (VODKA): Investigating the Nature of SDSS J0823+2418 at z = 1.81, A Likely Lensed Quasar
Authors: Arran C. Gross, Yu-Ching Chen, Adi Foord, Xin Liu, Yue Shen, Masamune Oguri, Andy Goulding, Hsiang-Chih Hwang, Nadia L. Zakamska, Yilun Ma, 逸伦 马, Liam Nolan
Figure caption: Archival SDSS spectrum of the SDSS J0823+2418 system, which has more wavelength coverage toward the observed-frame blue than the STIS or GMOS spectra. The presence of strong absorption lines around observed-frame 4500 and 4200 Å consistent with Mg and Fe suggests that an intervening absorber is located at z ∼ 0.62. These lines could be caused by relatively low column density gas in the intergalactic medium, but could be consistent with the foreground lensing galaxy.
Paper: ELVES. IV. The Satellite Stellar-to-halo Mass Relation Beyond the Milky Way
Authors: Shany Danieli, Jenny E. Greene, Scott Carlsten, Fangzhou Jiang, Rachael Beaton, Andy D. Goulding
Figure caption: The number of satellites, N sat, versus the stellar mass of the host inferred from its M  K -band group magnitude. Orange circles show the observed satellites of the 27 ELVES groups considered in this work, where satellites within r proj = 150 kpc are included, and upper error bars represent the uncertainty in N sat due to unconfirmed candidates (Section 2.1). The blue-shaded color map shows the number of realizations in N sat and M ⋆,host bins from simulating the satellite populations hosts galaxies (50 realizations per M ⋆,host), by populating their predicted subhalos (from SatGen) with our fiducial satellite SHMR. The observed and simulated trends are largely consistent with each other, though in some cases a large spread in N sat for a given M ⋆ suggests that the number of satellites might serve as a useful tracer for the physical processes that take place in these groups.