adsabs/AstroCLIMB huggingface dataset:
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: 2D histograms of simulated BNS (left) and NSBH (right) light curves for O4. We show light curves in u, g, r, i, z, y, J, H bands in order to include all the bands used by surveys considered in this work (ZTF, Rubin, and Gemini). In each panel, we plot three dash lines; on top the 10th percentile, at middle the 50th percentile and on bottom the 90th percentile. The color bar shows the number of detections in the different bands. For the observing run O5, see Figure 16, in Appendix B.1.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: 90% posterior credible intervals for the component masses for all CBCs in the GWTC-3 catalog (Abbott et al. 2023) study assuming uniform priors in detector-frame masses and fixed FAR about 0.25 year−1 (Abbott et al. 2023). Events classified by the LIGO-Virgo-KAGRA collaboration as BNSs, NSBHs, and BBHs are shown in dark violet, olive (dark yellowish-green), and orange, respectively. The ambiguously classified event GW190814 is shown in dark purple. The gray band indicates the approximate location of the purported lower-mass gap. GW190814 is the only event within this region at more than 90% credibility
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: This figure shows the simulated detections for O4. The upper panel shows the number of injections (CBCs from each population drawn from both distributions) in colored dots and the bar chart representing the number of events passing the S/N cut. The bottom panel shows the percentage of detection relative to the number injections for the two distributions. The colored dots represent the percentages of each population that passed the S/N, while the blue and green lines with respectively 0.83% and 0.22% are successively percentages of detection of all the events (BNS + NSBH + BBH) of the PBD/GWTC-3 (GWTC-3) and LRR distributions injected in our simulation. For O5, see Appendix A.1.2, Figure 15.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: Simulated mass distributions for O4. The left panel shows draws from the LRR distribution, and the right panel shows draws from the PBD/GWTC-3 (GWTC-3) distribution. The upper panels are the 2D mass distributions of the components of each CBC in the context of the detector, and the lower panels are the 2D primary mass and distance distributions. All axes are shown on a logarithmic scale. The color base shows the number of CBC events per pixel. For O5 results, see Appendix A.1.1, Figure 14.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: Flowchart of observing scenarios process. Here, μ = 1.33 M ⊙, and σ = 0.09 M ⊙; then, in LRR case, m represents the primary mass m 1 or secondary mass m 2, since they are drawn in the same way with m 2 ≤ m 1.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: Cutoffs between subpopulations of compact binary coalescences for both the GWTC-3 and LRR samples. It should be noted that the BHs in the LRR field are limited to be below 50 M ⊙, but are allowed to be as massive as 100 M ⊙ in the GWTC-3 distribution.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: The 1D mass distribution, p(m∣λ) on the interval [1, 100] M ⊙ for a specific choice of hyperparameters λ. See Table 7 in Appendix A.1, for the other parameters of the mass distribution.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The timescale of the conversion of NH3 → N2 (﹩{\tau }_{{\mathrm{NH}}_{3}};﹩ left column) and N2 → NH3 (﹩{\tau }_{{{\rm{N}}}_{2}};﹩ right column) for four different temperatures (750, 1250, 1750, and 2250 K) with five different metallicities (0.1, 1, 10, 100, and 1000× solar metallicity). The colored lines represent the timescale of the RLS, the corresponding temperature-pressure value, and the black dashed lines represent ﹩{\tau }_{{{\rm{H}}}_{2}}\,\times \,\tfrac{3[{{\rm{N}}}_{2}]}{{{\rm{H}}}_{2}}﹩. The solid black line represents ﹩{\tau }_{{\mathrm{NH}}_{3}}﹩ (left column) and ﹩{\tau }_{{{\rm{N}}}_{2}}﹩ (right column), labeled with the respective metallicity.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Variation of the equilibrium mole fraction for (a) NH3, (b) N2, and (c) HCN at 100 mbar and at 10 bar pressure with metallicity and temperature is shown. The solid black line represents the equal-abundance curve of NH3–N2, and the black dashed lines the constant contours of the mole fraction of the respective gas-phase species.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The equal-abundance curves of NH3–N2. The cyan-to-blue lines delimitate the region where NH3 (left) or N2 (right) is the dominant species. The metallicity value in the color bar corresponds to the respective color line in the plot. The dashed lines represent subsolar metallicity, and the solid lines supersolar metallicity.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The constant contour lines of ﹩{\tau }_{{{\rm{N}}}_{2}}﹩ (left) and ﹩{\tau }_{{\mathrm{NH}}_{3}}﹩ (right) are plotted for four different metallicities (0.1, 1, 10, and 1000× solar metallicity). The solid, dashed, dotted-dashed, and dotted lines show 0.1, 1, 10, and 1000 × solar metallicity, respectively. The colored lines from blue to yellow represent the constant contours of timescales in log10 scale for 0, 5, 10, 15, 20, 25, and 30.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The pressure–temperature range of different RLSs is shown for three different metallicities. Each color corresponds to the different RLSs in Figure 3. The top and bottom panels represent the RLS parameter space for the conversion of NH3 → N2 (﹩{\tau }_{{\mathrm{NH}}_{3}}﹩) and N2 → NH3 (﹩{\tau }_{{{\rm{N}}}_{2}}﹩).
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: The plots at the top are BNS distributions of the missed and found injections (on the left, BNS light curves observed by ZTF, and the right one shows the same observation in Rubin Observatory), as a function of the peak r-band absolute magnitude and 2D probability enclosed. We encode in the color bar and the transparency of the points the 3D probability of finding the transient as measured by simulated injections. The 1D histograms are marginalized versions of the 2D scatter plot, with the detected set in green, and missed set in red. The plots at the bottom are the same for the NSBH light curves. Those plots concern the run O5.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Major chemical pathways between ﹩\mathrm{HCN}\rightleftarrows {{\rm{NH}}}_{3}\rightleftarrows {{\rm{N}}}_{2}﹩ for the hydrogen-dominated atmosphere. The colored arrows, with the exception of the black arrows, represent the RLSs at different pressure–temperatures corresponding to the colored regions in Figure 4 and the RLS number in Table 1.
Paper: Updated Observing Scenarios and Multimessenger Implications for the International Gravitational-wave Networks O4 and O5
Authors: R. Weizmann Kiendrebeogo, Amanda M. Farah, Emily M. Foley, Abigail Gray, Nina Kunert, Anna Puecher, Andrew Toivonen, R. Oliver VandenBerg, Shreya Anand, Tomás Ahumada, Viraj Karambelkar, Michael W. Coughlin, Tim Dietrich, S. Zacharie Kam, Peter T. H. Pang, Leo P. Singer, Niharika Sravan
Figure caption: Those plots are the 1D histograms of the peak magnitudes in the ZTF and the Rubin observatory bands. On the left, we show ZTF BNS peak mag in the runs O4 (on top) and O5 (at bottom); then, on the right, the same plot for the case of Rubin Observatory. The black line shows the peak mag in all the bands of each telescope detected during the run O4 and O5 simulation.
Paper: Spectra of V1405 Cas at the Very Beginning Indicate a Low-mass ONeMg White Dwarf Progenitor
Authors: Kenta Taguchi, Keiichi Maeda, Hiroyuki Maehara, Akito Tajitsu, Masayuki Yamanaka, Akira Arai, Keisuke Isogai, Masaaki Shibata, Yusuke Tampo, Naoto Kojiguchi, Daisaku Nogami, Taichi Kato
Figure caption: Constraints on the conditions of the line-forming region in the (T, ρ) plane for (a,d) t = +9.88, (b), (e) t = +33.94, and (c), (f) t = +81.90 hr. The observed line luminosities are reproduced by the one-zone model on the colored curves, where different colors are used for different lines; a consistent solution is therefore found for the position of (T, ρ) where all the lines are largely overlapping with each other. For the non-detected lines, we place the limits in the (T, ρ) plane as shown by the colored dashed lines (with different colors for different lines), using the typical sensitivity of 1032 erg s−1 for the non-detection. The black line in each panel shows the constraint of the electron-scattering optical depth being unity, above which the line formation will become ineffective. The shaded area in each panel shows the forbidden region, where either at least one of the non-detection constraints or electron-scattering optical depth constraint is not satisfied. The left panels adopt the solar abundance for all the elements, while the right panels adopt the enhanced mass fractions for nitrogen and aluminum, by factors of 10 and 40 relative to the solar abundance, respectively.
Paper: Spectra of V1405 Cas at the Very Beginning Indicate a Low-mass ONeMg White Dwarf Progenitor
Authors: Kenta Taguchi, Keiichi Maeda, Hiroyuki Maehara, Akito Tajitsu, Masayuki Yamanaka, Akira Arai, Keisuke Isogai, Masaaki Shibata, Yusuke Tampo, Naoto Kojiguchi, Daisaku Nogami, Taichi Kato
Figure caption: Profiles of the Hβ and He I (7065 Å) lines of V1405 Cas. In each panel, the absorption minima at several epochs, measured using the SPLOT task of IRAF, are indicated by dashed lines. (a) Spectra around the Hβ line obtained with the VPH-blue grism of KOOLS-IFU and with HDS. The absorption minima on t = +9.88, +33.94, and +81.90 hr are at −1.6(1), −1.4(9), and −1.3(6) × 103 km s−1, respectively. For the HDS spectrum (t = +53.53 hr), the original high-resolution spectrum (gray) and the resolution-decreased one (black; same as Figure 2) are overplotted. (b) The same as panel (a), but for the He I (7065 Å) line obtained using the VPH-red grism. The absorption minima on t = +9.88, +33.94, and + 81.90 hr are at −1.6(6), −1.5(8), and −1.3(3) × 103 km s−1, respectively.
Paper: Broadband X-Ray Timing and Spectral Characteristics of the Accretion-powered Millisecond X-Ray Pulsar MAXIJ1816-195
Authors: Zhaosheng Li, Lucien Kuiper, Mingyu Ge, Maurizio Falanga, Juri Poutanen, Long Ji, Yuanyue Pan, Yue Huang, Renxin Xu, Liming Song, Jinlu Qu, Shu Zhang, Fangjun Lu, Shuang-Nan Zhang
Figure caption: The light curves of MAXI J1816−195 during its 2022 outburst. From top to bottom: the 100 s binned light curves from NICER, Insight-HXMT ME, and Insight-HXMT HE are displayed, respectively. The energy range of each light curve is indicated in each panel. The gray area marks the time of NuSTAR observation. Time intervals covering X-ray bursts are removed. The blue dashed lines represent the time interval that we used for the derivation of our timing models; see Table 1 and Section 3.
Paper: Broadband X-Ray Timing and Spectral Characteristics of the Accretion-powered Millisecond X-Ray Pulsar MAXIJ1816-195
Authors: Zhaosheng Li, Lucien Kuiper, Mingyu Ge, Maurizio Falanga, Juri Poutanen, Long Ji, Yuanyue Pan, Yue Huang, Renxin Xu, Liming Song, Jinlu Qu, Shu Zhang, Fangjun Lu, Shuang-Nan Zhang
Figure caption: The 0.8–210 keV broadband pulse-phase distributions of MAXI J1816−195 observed by NICER (panels (a)–(c); 0.8–10 keV), NuSTAR (panels (g)–(k); 3–79 keV), and Insight-HXMT (panels (d)–(f); 5–35 keV for ME; and panels (l)–(p); 20–210 keV for HE). In order to improve clarity, two cycles are shown. The error bars represent 1σ errors. The morphology is almost unchanged with energy. All profiles reach their maximum near phase ∼0.5.
Paper: Broadband X-Ray Timing and Spectral Characteristics of the Accretion-powered Millisecond X-Ray Pulsar MAXIJ1816-195
Authors: Zhaosheng Li, Lucien Kuiper, Mingyu Ge, Maurizio Falanga, Juri Poutanen, Long Ji, Yuanyue Pan, Yue Huang, Renxin Xu, Liming Song, Jinlu Qu, Shu Zhang, Fangjun Lu, Shuang-Nan Zhang
Figure caption: The unabsorbed spectra of MAXI J1816−195 from NICER, NuSTAR FPMA, NuSTAR FPMB, Insight-HXMT ME, and Insight-HXMT HE in the 1–150 keV energy range. The fitting model is constant×tbabs (Gaussian+Gaussian+diskbb+compps). The black dashed lines represent the two Gaussian lines. The best-fit model is plotted as black solid line. The disk blackbody and compps components are shown in dotted and dashed–dotted–dotted–dotted lines, respectively.
Paper: Broadband X-Ray Timing and Spectral Characteristics of the Accretion-powered Millisecond X-Ray Pulsar MAXIJ1816-195
Authors: Zhaosheng Li, Lucien Kuiper, Mingyu Ge, Maurizio Falanga, Juri Poutanen, Long Ji, Yuanyue Pan, Yue Huang, Renxin Xu, Liming Song, Jinlu Qu, Shu Zhang, Fangjun Lu, Shuang-Nan Zhang
Figure caption: Pulse-phase residuals of Insight-HXMT HE (open black triangles; 20–35 keV), Insight-HXMT ME (open orange squares; 10–20 keV), and NICER (open aqua diamonds; 1.8–10 keV) ToAs with respect to a two-parameter timing model (including a quadratic/spinup term) valid for the range MJD 59741.9–59760.6. These models are based on solely Insight-HXMT HE ToAs (black data points). The interval bounded by the two blue dashed lines represents this time interval that has been used to derive the timing models given in Table 1. Note that there are no ToA measurements beyond MJD 59760.6 for Insight-HXMT HE (and ME), contrary to NICER.
Paper: Broadband X-Ray Timing and Spectral Characteristics of the Accretion-powered Millisecond X-Ray Pulsar MAXIJ1816-195
Authors: Zhaosheng Li, Lucien Kuiper, Mingyu Ge, Maurizio Falanga, Juri Poutanen, Long Ji, Yuanyue Pan, Yue Huang, Renxin Xu, Liming Song, Jinlu Qu, Shu Zhang, Fangjun Lu, Shuang-Nan Zhang
Figure caption: Left: the fractional amplitude of various harmonics: (1) fundamental overtone (black crosses) and (2) first overtone (red crosses) as a function of energy using background-corrected data from NICER (filled squares), NuSTAR (triangles), Insight-HXMT ME (filled circles), and Insight-HXMT HE (open circles). Right: the phase angle (in units of radians/2π) as a function of energy for the two Fourier components, the fundamental (in black) and the first overtone (in red), which are independent of the background-subtraction method.
Paper: Broadband X-Ray Timing and Spectral Characteristics of the Accretion-powered Millisecond X-Ray Pulsar MAXIJ1816-195
Authors: Zhaosheng Li, Lucien Kuiper, Mingyu Ge, Maurizio Falanga, Juri Poutanen, Long Ji, Yuanyue Pan, Yue Huang, Renxin Xu, Liming Song, Jinlu Qu, Shu Zhang, Fangjun Lu, Shuang-Nan Zhang
Figure caption: The fitted results of joint NICER and Insight-HXMT spectra by the model constant×tbabs (Gaussian + Gaussian + diskbb + compps). From top to bottom, the bolometric flux (in units of 10−8 erg cm−2 s−1), the hydrogen column density (in 1022 cm−2), the electron temperature (in keV), the optical depth, the temperature of the disk blackbody (in keV), and the reduced χ 2 are shown.
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Evolution of galaxies in sSFR–M * (upper panels) and ΣSFR–M * diagrams (lower panels). For low-redshift samples we show only the main-sequence galaxies. In the sSFR–M * diagrams the slope of the main sequence stays more or less the same, whereas the ΣSFR–M * diagrams reveal a change—there was higher SF activity of massive galaxies compared to less massive ones in the past, consistent with a bulge buildup of those systems. Dashed lines in the lower panels signify the upper boundary of the low-redshift transition region. At higher redshift this boundary is higher and would have encompassed today’s main-sequence galaxies. The dotted lines represent the threshold for full quenching, which is independent of the redshift.
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Low-redshift galaxy samples shown on the sSFR–M * (left) and ΣSFR–M * diagrams (right). The lower panels in both figures show the subset of galaxies that form the main sequence. The character of the main sequence changes when going from sSFR to ΣSFR–it becomes flatter, while remaining tight (width, in dex, given in the panels). Once the measure of SF activity is decoupled from the past SF history by using ΣSFR, the SF level is not strongly mass dependent.
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Trends of the Sérsic index as a function of sSFR (upper panels) and ΣSFR (lower panels), at different redshifts. Galaxies with today’s values of sSFR or ΣSFR characteristic of the main sequence would be found below the main sequence at high redshift and, like transitional galaxies today, would have, on average, a high Sérsic index. This suggests that morphological transformation is associated with a relative suppression of sSFR or ΣSFR, but to values that would still be considered quite high by today’s norms. The red dashed line corresponds to an n = 4 de Vaucouleurs profile, and the blue line corresponds to n = 2.5, an approximate dividing line between galaxies with and without a central spheroid. Shown are galaxies with ﹩10\lt \mathrm{log}{M}_{* }\lt 11﹩. Curves represent the 16th percentile, the mean, and the 84th percentile in each x-axis bin. Curves at z ∼ 1 and 2 are smoothed to mitigate low numbers of objects.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: Examples of the H I SPS for four different regions with individual contributions from Equation (4). Within each panel, the gray, yellow, red, blue, and green data points represent the beam, total noise, observed, observed-beam, and final SPS, respectively. Furthermore, the dashed lines in the figure indicate the range of fitting for both large and small scales as 1.°5 and 16′, which corresponds to spatial frequencies k = 10−2 arcmin–1 to ∼6 × 10−2 arcmin−1.
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Relationship between the isophotal radius (in kiloparsecs) and (a) the effective radius (also in kiloparsecs), (b) the stellar mass (in solar masses), and (c) a combination of the effective size and stellar mass that minimizes scatter (from left to right). Isophotal size is poorly correlated with either the effective size or the stellar mass, but is tightly correlated with the linear combination of the two (in logarithm), providing a way to precisely predict the isophotal radius if it is not available (see Equation (6)). Standard deviations of the residuals around the best linear fit (dashed line) are given in the panels. Solid lines show a 1:1 relation where applicable. All of the low-redshift samples in this and subsequent figures come from GSWLC-M2.
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Main-sequence merger pairs (interacting galaxies) overplotted on the general low-redshift main-sequence population. The same galaxies are shown on the sSFR–M * (left) and ΣSFR–M * diagrams (right). The merger pairs serve as proxies for starbursts and come from Darg et al. (2010). The merging galaxies have a similar average offset (blue line) from the ridge of the overall main sequence (red line) in both cases; however, because there is no mass dependence, selecting starbursts by the SFR surface density is obviously much cleaner than doing so based on the sSFR.