adsabs/AstroCLIMB huggingface dataset:
Paper: Shedding Light on the Origin of the Broken Misaligned Circumtriple Disk around GW Ori
Authors: Jeremy L. Smallwood, Stephen H. Lubow, Rebecca G. Martin, Rebecca Nealon
Figure caption: The disk surface density, Σ, as a function of radius, r, for initial circumtriple disk misalignment of i0 = 38∘ (left plot) and i0 = 28∘ (right plot). The initial surface density profile is given by the flat black line. The thin yellow and thick purple lines denote H/r = 0.02 and H/r = 0.05, respectively. For each disk misalignment, the disk breaks when H/r = 0.02.
Paper: Shedding Light on the Origin of the Broken Misaligned Circumtriple Disk around GW Ori
Authors: Jeremy L. Smallwood, Stephen H. Lubow, Rebecca G. Martin, Rebecca Nealon
Figure caption: The observationally estimated disk aspect ratio, H/r, as a function of disk radius, r, for GW Ori from Equation (5). The black double-hatched area represents the orbital extent of the AB-C binary. The red single-hatched area denotes the area where the tidal torque truncates the disk.
Paper: GRB 241107A: A Giant Flare from a Close-by Extragalactic Magnetar?
Authors: James Craig Rodi, Dominik Patryk Pacholski, Sandro Mereghetti, Edoardo Arrigoni, Angela Bazzano, Lorenzo Natalucci, Ruben Salvaterra, Pietro Ubertini
Figure caption: Background-subtracted light curves of GRB 241107A in three energy bands, with T0 = 2024-11-07 23:30:00 UT. The ISGRI (40–200 keV) light curve has been binned to have at least 18 counts in each bin ((A) panel). The PICsIT light curves (200–468.2 keV, (B) panel and 468.2–2600 keV, (C) panel) have the original bin size of 3.9 ms. Panel (D) shows the evolution of Ep during the burst.
Paper: GRB 241107A: A Giant Flare from a Close-by Extragalactic Magnetar?
Authors: James Craig Rodi, Dominik Patryk Pacholski, Sandro Mereghetti, Edoardo Arrigoni, Angela Bazzano, Lorenzo Natalucci, Ruben Salvaterra, Pietro Ubertini
Figure caption: Pan-STARRS1 optical image of the location of GRB 241107A  with the i band, r band, and g band used as RGB colors. The circle with radius 3′ is the IBIS/ISGRI position (90% c.l.). The galaxy PGC 86046 is clearly visible at coordinates R.A. = 7:25:22, decl. = –24:28:23.
Paper: GRB 241107A: A Giant Flare from a Close-by Extragalactic Magnetar?
Authors: James Craig Rodi, Dominik Patryk Pacholski, Sandro Mereghetti, Edoardo Arrigoni, Angela Bazzano, Lorenzo Natalucci, Ruben Salvaterra, Pietro Ubertini
Figure caption: Position of GRB 241107A (red square) in the Ep vs. Eiso plane. The sample of short GRBs (blue) is taken from P. Y. Minaev & A. S. Pozanenko (2020). The three confirmed magnetar giant flares and the extragalactic MGF candidates are indicated by the green stars (data from D. P. Pacholski et al. 2024 and references therein and D. S. Svinkin et al. 2016).
Paper: GRB 241107A: A Giant Flare from a Close-by Extragalactic Magnetar?
Authors: James Craig Rodi, Dominik Patryk Pacholski, Sandro Mereghetti, Edoardo Arrigoni, Angela Bazzano, Lorenzo Natalucci, Ruben Salvaterra, Pietro Ubertini
Figure caption: Time-averaged IBIS spectrum of GRB 241107A (from T0 + 0.17 s to T0 + 0.40 s). ISGRI data are plotted as black diamonds and PICsIT data as red triangles. The best-fit cutoff power-law model is overplotted as a solid blue line.
Paper: GRB 241107A: A Giant Flare from a Close-by Extragalactic Magnetar?
Authors: James Craig Rodi, Dominik Patryk Pacholski, Sandro Mereghetti, Edoardo Arrigoni, Angela Bazzano, Lorenzo Natalucci, Ruben Salvaterra, Pietro Ubertini
Figure caption: Confidence contours of the joint ISGRI+PICsIT spectra for the peak (T0 + 0.17–T0 + 0.20, solid blue line) and tail (T0+0.20–T0+0.40, dashed red line) of the burst. The contours represent confidence levels of 68%, 90%, and 99%.
Paper: Long-term Radio Monitoring of the Fast X-Ray Transient EP 240315a: Evidence for a Relativistic Jet
Authors: Roberto Ricci, Eleonora Troja, Yu-Han Yang, Muskan Yadav, Yuan Liu, Hui Sun, Xuefeng Wu, He Gao, Bing Zhang, Weimin Yuan
Figure caption: Smoothed double power-law fit to the light curve of the 5.5 GHz (upper panel) and 9 GHz (middle panel) radio data. The lower panel shows the temporal evolution of the radio spectral index. Downward triangles represent 3σ upper limits from ATCA. The open square shows the MeerKAT data point, shifted from 3 to 5.5 GHz.
Paper: Long-term Radio Monitoring of the Fast X-Ray Transient EP 240315a: Evidence for a Relativistic Jet
Authors: Roberto Ricci, Eleonora Troja, Yu-Han Yang, Muskan Yadav, Yuan Liu, Hui Sun, Xuefeng Wu, He Gao, Bing Zhang, Weimin Yuan
Figure caption: Broadband modeling results. Left panel: multiwavelength light curves overlaid with the best-fit model. Optical and X-ray data are from Y. Liu et al. (2024). Downward arrows represent upper limits. Empty points are used for observations in the exclusion time span (250–450 ks after trigger time). Right panel: corner plot of the posterior distribution of the modeled parameters. In both panels Case 1 is presented.
Paper: Long-term Radio Monitoring of the Fast X-Ray Transient EP 240315a: Evidence for a Relativistic Jet
Authors: Roberto Ricci, Eleonora Troja, Yu-Han Yang, Muskan Yadav, Yuan Liu, Hui Sun, Xuefeng Wu, He Gao, Bing Zhang, Weimin Yuan
Figure caption: Radio luminosity light curve of EP 240315A compared with a sample of cosmological GRBs (black) and subenergetic GRBs (gray) (P. Chandra & D. A. Frail 2012; S. Dichiara et al. 2022).
Paper: Timescales of Solar System Formation Based on Al–Ti Isotope Correlation by Supernova Ejecta
Authors: Tsuyoshi Iizuka, Yuki Hibiya, Satoshi Yoshihara, Takehito Hayakawa
Figure caption: Titanium isotopes as a proxy for the nucleosynthetic heterogeneity. (a) ε46Ti–ε50Ti variation diagram for solar system objects. Mixing trends between the angrite source reservoir and five potential stellar Ti sources are shown for comparison: postexplosion compositions of Type Ia supernovae (K. Maeda et al. 2010) and 15 Mʘ CCSNe (T. Rauscher et al. 2002), an AGB s-process component (U. Battino et al. 2019), and weak s-process components in the He-burning core (L. S. The et al. 2000) and C-burning shell (M. Pignatari et al. 2010) in massive stars. The ticks on the mixing line with the C-shell component denote the dilution factor Δd of the ejecta at 10–4 intervals. The Ti isotope data are listed in Supporting Data. (b) (26Al/27Al)0 vs. ε50Ti for the meteoritic samples. The (26Al/27Al)0 values were obtained by projecting (26Al/27Al)I of the individual meteorites onto the time of CAI formation at 4567.30 Ma using their Pb–Pb ages and the decay rate of 26Al (Table A1). Solid and dashed lines represent the regression and 95% confidence intervals of the data, respectively.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Timescales of Solar System Formation Based on Al–Ti Isotope Correlation by Supernova Ejecta
Authors: Tsuyoshi Iizuka, Yuki Hibiya, Satoshi Yoshihara, Takehito Hayakawa
Figure caption: Schematic timeline of solar system formation. The ages shown are relative to the time of CAI formation. The Sun was born in association with a ∼25 Mʘ star. The protosolar clumpy cloud developed along the stellar-wind-blown bubble was polluted by ejecta from the CCSN explosion at around –0.9 Myr through dust injection. The injected dust would be sputtered and release CCSN-derived nuclides including 26Al and Ti isotopes in the cloud, followed by condensation of these nuclides as mantles (blue) onto preexisting dust of different stellar origins (red). Within the nascent inner disk around the proto-Sun, these mantles would be preferentially destroyed by thermal processing, rendering the residual solids depleted in CCSN-derived nuclides. Besides, CAIs were condensed from the complementary gaseous reservoir rich in these nuclides and were transported to the outer disk by protostellar outflow. The parent asteroids of noncarbonaceous (NC) and carbonaceous chondrites (CC) were accreted in the inner and outer disks at ∼0.5 and ∼3.0 Myr, likely through the pileup of inward-drifting pebbles around the snow line that has migrated outward (T. Lichtenberg et al. 2021). Consequently, carbonaceous meteorites, in particular those bearing CAIs, are more enriched in CCSN-derived nuclides than the noncarbonaceous ones.
Paper: Timescales of Solar System Formation Based on Al–Ti Isotope Correlation by Supernova Ejecta
Authors: Tsuyoshi Iizuka, Yuki Hibiya, Satoshi Yoshihara, Takehito Hayakawa
Figure caption: (26Al/27Al)I vs. Pb–Pb age plots for the meteoritic samples. The solid line represents the canonical 26Al decay line defined by CAIs (K. K. Larsen et al. 2011). The vertical dashed line indicates the time of CAI formation (4567.30 Ma; Y. Amelin et al. 2010; J. N. Connelly et al. 2012). All the Pb–Pb ages were calculated using the measured 238U/235U of the individual samples. Error bars represent 2σ. The data are listed in Table A1.
Paper: Timescales of Solar System Formation Based on Al–Ti Isotope Correlation by Supernova Ejecta
Authors: Tsuyoshi Iizuka, Yuki Hibiya, Satoshi Yoshihara, Takehito Hayakawa
Figure caption: Accretion chronology of ordinary and carbonaceous chondrite parent bodies. The colored symbols represent the ages calibrated using the Al–Ti isotope correlation, whereas the open symbols represent the reported ages without the calibration. The numbers next to the symbols indicate the assumed or inferred radii (km) of the parent bodies. The reported ages were from P. M. Doyle et al. (2015) for L, CO, and CV (20–50 km radius); S. Henke et al. (2012) for H; K. Jogo et al. (2017) for CV (110–150 km radius); W. Fujiya et al. (2012) for CM; and W. Fujiya et al. (2013) for CI chondrites.
Paper: Timescales of Solar System Formation Based on Al–Ti Isotope Correlation by Supernova Ejecta
Authors: Tsuyoshi Iizuka, Yuki Hibiya, Satoshi Yoshihara, Takehito Hayakawa
Figure caption: CI-chondrite- and Al-normalized major and trace element abundances of chondrites. The data are plotted against the 50% condensation temperature of a solar composition gas at 10−4 bars (K. Lodders 2003). The data sources are H. Palme & H. O’Neill (2014) for CI; D. S. Lauretta et al. (2009) for CB; A. Bischoff et al. (1993) for CH; N. Braukmüller et al. (2018) for CR, CV, CK, CM, and CO; J. T. Wasson & G. W. Kallemeyn (1988) for H, L, and LL chondrites; and J. T. Wasson & G. W. Kallemeyn (1988) and D. C. Lee & A. N. Halliday (2000) for EH and EL chondrites.
Paper: Transonic Turbulence and Density Fluctuations in the Near-Sun Solar Wind
Authors: L.-L. Zhao, A. Silwal, X. Zhu, H. Li, G. P. Zank
Figure caption: The left panel shows the normalized histograms that represent the probability density function (PDF) of the turbulent sonic Mach number Mt for three heliocentric distance ranges observed by PSP and SolO. The histogram is normalized so that the area under each curve is equal to 1. The right panel shows the radial distance dependence of the bulk flow Alfvén Mach number MA, turbulent sonic Mach number Mt, and the amplitude of velocity fluctuation δV calculated at 10 minute intervals from the PSP data set.
Paper: Transonic Turbulence and Density Fluctuations in the Near-Sun Solar Wind
Authors: L.-L. Zhao, A. Silwal, X. Zhu, H. Li, G. P. Zank
Figure caption: The left panel shows a 2D histogram of Alfvén Mach number MA and proton beta β from PSP measurements. The right panel shows a 2D histogram of MA and Mt, with the color map indicating the PDF of bin counts. The PDFs of MA and Mt are shown on the top and right, respectively.
Paper: Transonic Turbulence and Density Fluctuations in the Near-Sun Solar Wind
Authors: L.-L. Zhao, A. Silwal, X. Zhu, H. Li, G. P. Zank
Figure caption: Radial evolution of the scaling relation between the density fluctuation δρ/ρ0 and Mt observed by PSP and SolO from 10 to 80 R⊙. The panels from left to right show the scaling of density fluctuations in radial distances of 10–20 R⊙, 20–40 R⊙, 40–60 R⊙, and 60–80 R⊙, respectively. Each panel represents a 2D histogram of δρ/ρ0 vs. Mt, color coded by the sampling angle θVB. The red asterisk in each panel indicates the average values of Mt and δρ/ρ0 in each distance range.
Paper: High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons
Authors: Xu Yang, Meiqi Wang, Andrew Cao, Kaifan Ji, Vasyl Yurchyshyn, Jiong Qiu, Sijie Yu, Jinhua Shen, Wenda Cao
Figure caption: Multiwavelength flare light curves and flare ribbons. Panels (c1), (c2), and (c3) present a BFI/TiO running difference image, an HMI/Ic base difference image, and a VIS/Hα line center running difference image, respectively. Three WLF ribbons are indicated by the yellow rectangles. The red and orange contours indicate 5% enhancement in BFI/TiO and HMI/Ic. The cyan contours indicate 30% enhancement in VIS/Hα. Panels (a1)–(a3) present the correspondence between Fermi/HXR (green solid, multiple energy bands) and averaged WL intensity enhancements in BFI/TiO (blue solid) and HMI/Ic (red dotted–dashed) in the yellow areas. The background variation from a relatively quiet area (purple square in panel (c1)) has been subtracted in each wavelength. The HMI/Ic light curve is plotted in an adjusted anonymous scale to match the BFI/TiO amplitude. Panels (b1)–(b3) present the Fermi/HXR light curve in multiple energy bands and averaged EOVSA 14.9 GHz light curve (cyan solid) in each high-frequency radio source (K1, K2r, K3).
Paper: High-resolution Observations of an X-1.0 White-light Flare with Moving Flare Ribbons
Authors: Xu Yang, Meiqi Wang, Andrew Cao, Kaifan Ji, Vasyl Yurchyshyn, Jiong Qiu, Sijie Yu, Jinhua Shen, Wenda Cao
Figure caption: Zoom-in images at K3. Panels (a1)–(a3) and (c1) present the lower WLF ribbon resolved by BFI/TiO and HMI/Ic. Panels (b1)–(b3) displays flare ribbon in the chromosphere recorded by VIS/Hα red-wing images. Yellow contours in panels (a1)–(a3) and (b1)–(b3) indicate the leading edge of the Hα flare ribbon. Green contours in panel (c3) indicate the positive polarities of the LOS magnetic field. The cyan arrows in panels (a3) and (b3) indicate the spatial evolution of this flare ribbon. Panels (c2) and (c3) are TiO and Hα time–distance slices made along the cyan arrows.
Paper: Transonic Turbulence and Density Fluctuations in the Near-Sun Solar Wind
Authors: L.-L. Zhao, A. Silwal, X. Zhu, H. Li, G. P. Zank
Figure caption: The wavelet power spectral density (PSD) of the total trace magnetic fluctuations (left panel) and proton density fluctuations (right panel) for different turbulent sonic Mach number Mt ranges. The black dashed lines indicate the power-law fits in the frequency range from 10−2 to 10−1 Hz.
Paper: Transonic Turbulence and Density Fluctuations in the Near-Sun Solar Wind
Authors: L.-L. Zhao, A. Silwal, X. Zhu, H. Li, G. P. Zank
Figure caption: The left panel shows the joint distribution function of the cross correlation between the magnetic field magnitude fluctuations δ∣B∣/∣B∣ and proton density fluctuations δnp/np using the present PSP data set. The right panel shows the probability density function (PDF) of the normalized density fluctuations in three different radial distance ranges using both PSP and SolO data sets. The solid curves represent the lognormal distribution fits.
Paper: Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at 0.7 ≲ z ≲ 9.3 with NIRSpec High-resolution Spectroscopy 
Authors: Sijia Li, Xin Wang, Yuguang Chen, Tucker Jones, Tommaso Treu, Karl Glazebrook, Xianlong He, Alaina Henry, Xiao-Lei Meng, Takahiro Morishita, Guido Roberts-Borsani, Lilan Yang, Hao-Ran Yu, Antonello Calabrò, Marco Castellano, Nicha Leethochawalit, Benjamin Metha, Themiya Nanayakkara, Namrata Roy, Benedetta Vulcani
Figure caption: Observed spectra and emission line fitting for GLASS-40202 at z = 3.7317 (top) and GLASS-20006 at z = 1.6751 (bottom). In both cases, the top two panels illustrate the emission line fits for the [O II] and [S II] doublets. The blue stepped lines represent the observed spectra, with the blue boxes indicating 1σ uncertainties. The best-fit single Gaussian for each line is shown in red, while the green curves represent the best-fit double Gaussian model for the doublets. The orange steps display the residuals of the fit. The bottom panels present the full observed spectrum of each galaxy, with prominent emission lines labeled. Inset images show color-composite images of the galaxies.
Paper: Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at 0.7 ≲ z ≲ 9.3 with NIRSpec High-resolution Spectroscopy 
Authors: Sijia Li, Xin Wang, Yuguang Chen, Tucker Jones, Tommaso Treu, Karl Glazebrook, Xianlong He, Alaina Henry, Xiao-Lei Meng, Takahiro Morishita, Guido Roberts-Borsani, Lilan Yang, Hao-Ran Yu, Antonello Calabrò, Marco Castellano, Nicha Leethochawalit, Benjamin Metha, Themiya Nanayakkara, Namrata Roy, Benedetta Vulcani
Figure caption: Observed high-resolution (R ~ 2700) and synthetic medium-resolution (R ~ 1000) spectroscopy of the [O II] doublets of GLASS-20006. The top panel shows the original spectrum of the [O II] doublets secured with the high-resolution G140H grating. In the bottom panel, we show a smoothed spectrum with effective resolution downgraded to that similar to the medium-resolution G140M grating, to which we also perform emission line profile fitting. We fit both doublets shown in the green Gaussian profile with their addition in green. We find that the value of ne estimated from the synthetic medium-resolution data significantly deviates from that given by the original high-resolution spectrum. This test highlights the caveat of estimating ne from the [O II] doublets marginally resolved by the JWST NIRSpec medium-resolution spectroscopy.
Paper: Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at 0.7 ≲ z ≲ 9.3 with NIRSpec High-resolution Spectroscopy 
Authors: Sijia Li, Xin Wang, Yuguang Chen, Tucker Jones, Tommaso Treu, Karl Glazebrook, Xianlong He, Alaina Henry, Xiao-Lei Meng, Takahiro Morishita, Guido Roberts-Borsani, Lilan Yang, Hao-Ran Yu, Antonello Calabrò, Marco Castellano, Nicha Leethochawalit, Benjamin Metha, Themiya Nanayakkara, Namrata Roy, Benedetta Vulcani
Figure caption: Comparison of the ISM electron density derived from the [O II] λλ3726, 3729 and [S II] λλ6718, 6732 doublet flux ratios. In the left panel, the orange circles denote ne measured using both tracers, assuming a fiducial electron temperature of Te([O II])=Te([S II]) = 10,000 K, with the error bars showing 1σ uncertainties. The 1σ upper limits are marked by triangles. We also estimate Te([O II]) from the detection or 1σ upper limit of the [O III] λ4363 auroral line using Equation (4), listed in green numbers, and then derive the ne constraints, marked in green symbols. In both panels, the gray points show the comparison for planetary nebulae in the Milky Way (R. L. Kingsburgh & J. English 1992), the yellow dots mark the ne comparison in individual H II regions within a local starburst galaxy (D. Fernández-Arenas et al. 2023), and the purple shaded band corresponds to the 1σ confidence interval of the ne comparison of a sample of local H II regions analyzed in R. L. Sanders et al. (2016). In the right panel, we instead color code our results using their corresponding sSFR measurements (see Section 3.6).
Paper: Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at 0.7 ≲ z ≲ 9.3 with NIRSpec High-resolution Spectroscopy 
Authors: Sijia Li, Xin Wang, Yuguang Chen, Tucker Jones, Tommaso Treu, Karl Glazebrook, Xianlong He, Alaina Henry, Xiao-Lei Meng, Takahiro Morishita, Guido Roberts-Borsani, Lilan Yang, Hao-Ran Yu, Antonello Calabrò, Marco Castellano, Nicha Leethochawalit, Benjamin Metha, Themiya Nanayakkara, Namrata Roy, Benedetta Vulcani
Figure caption: Redshift evolution of the ISM electron density (ne) of the high-redshift galaxies analyzed in this work. The ne measurements based on the low-ionization emission line flux ratios of the [O II] and [S II] doublets are represented by the green and orange circles, respectively. The blue stars correspond to the running median ne values measured in the five redshift bins. The hexagon shows the median measurement from the SDSS galaxies at z ~ 0. The black dashed line marks our best-fit redshift evolution with 1σ uncertainties of ﹩{n}_{{\rm{e}}}\propto {(1+z)}^{0.98{4}_{-0.909}^{+1.085}}﹩ to our measurements at high redshifts and the SDSS measurement at z ~ 0. The thin gray lines denote 50 random draws based on the 1σ uncertainties of the linear regression. We note that our constrained relation between ne and z is also compatible with no redshift evolution of ne across z ~ 2 to z ~ 9.
Paper: Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at 0.7 ≲ z ≲ 9.3 with NIRSpec High-resolution Spectroscopy 
Authors: Sijia Li, Xin Wang, Yuguang Chen, Tucker Jones, Tommaso Treu, Karl Glazebrook, Xianlong He, Alaina Henry, Xiao-Lei Meng, Takahiro Morishita, Guido Roberts-Borsani, Lilan Yang, Hao-Ran Yu, Antonello Calabrò, Marco Castellano, Nicha Leethochawalit, Benjamin Metha, Themiya Nanayakkara, Namrata Roy, Benedetta Vulcani
Figure caption: The relationships between line flux ratios and sSFR of our sample galaxies. The left panel shows the [O II] λ3726/[O II]λ3729 flux ratio, and the right panel shows [S II]λ6718/[S II]λ6732. Note that the [O II] λλ3726, 3729 doublets are well resolved by our GLASS-JWST NIRSpec MOS spectroscopy taken with the high-resolution gratings. The SFR values shown in both panels are measured from the reddening-corrected Balmer line fluxes. The color coding represents z as shown by the color bar on the right. In both panels, the dark and thin gray lines correspond to the best fit and 50 random draws from the linear regression. The p-value in the left and right panels is 0.22 and 0.44, respectively.
Paper: Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at 0.7 ≲ z ≲ 9.3 with NIRSpec High-resolution Spectroscopy 
Authors: Sijia Li, Xin Wang, Yuguang Chen, Tucker Jones, Tommaso Treu, Karl Glazebrook, Xianlong He, Alaina Henry, Xiao-Lei Meng, Takahiro Morishita, Guido Roberts-Borsani, Lilan Yang, Hao-Ran Yu, Antonello Calabrò, Marco Castellano, Nicha Leethochawalit, Benjamin Metha, Themiya Nanayakkara, Namrata Roy, Benedetta Vulcani
Figure caption: The distribution of M* and SFR for the galaxies in our sample. The data points are color-coded by their redshifts. The solid thick lines indicate the star-forming main sequence at the corresponding redshifts adopted from J. S. Speagle et al. (2014). Our galaxy samples are represented by large squares and are roughly representative of the star-forming main sequence at the corresponding redshifts.
Paper: Early Results from GLASS-JWST. XXV. Electron Density in the Interstellar Medium at 0.7 ≲ z ≲ 9.3 with NIRSpec High-resolution Spectroscopy 
Authors: Sijia Li, Xin Wang, Yuguang Chen, Tucker Jones, Tommaso Treu, Karl Glazebrook, Xianlong He, Alaina Henry, Xiao-Lei Meng, Takahiro Morishita, Guido Roberts-Borsani, Lilan Yang, Hao-Ran Yu, Antonello Calabrò, Marco Castellano, Nicha Leethochawalit, Benjamin Metha, Themiya Nanayakkara, Namrata Roy, Benedetta Vulcani
Figure caption: The relationship between ne and sSFR of all galaxies in our sample. The color coding represents z, with the same scale shown in Figure 3. The thin gray lines mark 50 random draws from the linear regression, with the dark gray line representing the best fit.