adsabs/AstroCLIMB huggingface dataset:
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High-contrast Imaging of the Exoplanet HIP 65426 b from 2 to 16 μm
Authors: Aarynn L. Carter, Sasha Hinkley, Jens Kammerer, Andrew Skemer, Beth A. Biller, Jarron M. Leisenring, Maxwell A. Millar-Blanchaer, Simon Petrus, Jordan M. Stone, Kimberly Ward-Duong, Jason J. Wang, Julien H. Girard, Dean C. Hines, Marshall D. Perrin, Laurent Pueyo, William O. Balmer, Mariangela Bonavita, Mickael Bonnefoy, Gael Chauvin, Elodie Choquet, Valentin Christiaens, Camilla Danielski, Grant M. Kennedy, Elisabeth C. Matthews, Brittany E. Miles, Polychronis Patapis, Shrishmoy Ray, Emily Rickman, Steph Sallum, Karl R. Stapelfeldt, Niall Whiteford, Yifan Zhou, Olivier Absil, Anthony Boccaletti, Mark Booth, Brendan P. Bowler, Christine H. Chen, Thayne Currie, Jonathan J. Fortney, Carol A. Grady, Alexandra Z. Greebaum, Thomas Henning, Kielan K. W. Hoch, Markus Janson, Paul Kalas, Matthew A. Kenworthy, Pierre Kervella, Adam L. Kraus, Pierre-Olivier Lagage, Michael C. Liu, Bruce Macintosh, Sebastian Marino, Mark S. Marley, Christian Marois, Brenda C. Matthews, Dimitri Mawet, Michael W. McElwain, Stanimir Metchev, Michael R. Meyer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Eric Pantin, Andreas Quirrenbach, Isabel Rebollido, Bin B. Ren, Glenn Schneider, Malavika Vasist, Kadin Worthen, Mark C. Wyatt, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gabriele Cugno, Matthew De Furio, Trent J. Dupuy, Samuel M. Factor, Jacqueline K. Faherty, Michael P. Fitzgerald, Kyle Franson, Eileen C. Gonzales, Callie E. Hood, Alex R. Howe, Masayuki Kuzuhara, Anne-Marie Lagrange, Kellen Lawson, Cecilia Lazzoni, Ben W. P. Lew, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Raquel A. Martinez, Johan Mazoyer, Paulina Palma-Bifani, Sascha P. Quanz, Jea Adams Redai, Matthias Samland, Joshua E. Schlieder, Motohide Tamura, Xianyu Tan, Taichi Uyama, Arthur Vigan, Johanna M. Vos, Kevin Wagner, Schuyler G. Wolff, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang
Figure caption: As in Figure 3, except for the NIRCam F250M, F300M, F356W, F410M, and F444W filters. Here, we show subtractions using the maximum number of PCA modes for ADI, RDI, and ADI+RDI, respectively. The F250M subtracted images have been smoothed as described in Section 2.
Paper: Investigating Possible Binarity for GJ 229B
Authors: Alex R. Howe, Avi M. Mandell, Michael W. McElwain
Figure caption: Goodness of fit to observed spectra of GJ 229B of our binary forward model grids, with a total mass of 71 M  J , calculated from the Sonora–Bobcat (S-B) models (Marley et al. 2017) (left) and from out APOLLO forward models (right). For the primary, the cutoff on the left edge is based on a mass greater than 50% of the total mass of the system, and the cutoff on the right is based on an age less than a Hubble time. For the secondary, the low temperature cutoff is based on the limitations of the molecular cross-section tables used by APOLLO. The outermost contours are representative of our adopted 1σ uncertainties, although they are slightly different for each local minimum.
Paper: Investigating Possible Binarity for GJ 229B
Authors: Alex R. Howe, Avi M. Mandell, Michael W. McElwain
Figure caption: Same as Figure 1, except with a total mass of 60 M  J .
Paper: Turbulence-supported Massive Star Envelopes
Authors: William C. Schultz, Lars Bildsten, Yan-Fei Jiang, 燕飞 姜
Figure caption: Comparison of radial profiles of the volume weighted average temperature, 〈T〉 V  (dotted lines), and the temperature extracted from the internal energy, 〈T〉 E  (solid lines), for the five models. The shaded color regions show the 95% spatial variability in a single temporal snapshot. Vertical colored lines show the radii where 〈τ〉 E  = 1 (dotted) and ﹩L/4\pi {r}^{2}=\sigma \langle T{\rangle }_{E}^{4}﹩ (dashed). The gray shaded regions denote where the average entropy gradient is negative, signifying a CZ. Temperature profiles from MESA models of similar stars to M13TAMS, M35ZAMS, and M35MMS are plotted in black dotted lines with their photospheric radii shown by the vertical gray dashed lines.
Paper: Turbulence-supported Massive Star Envelopes
Authors: William C. Schultz, Lars Bildsten, Yan-Fei Jiang, 燕飞 姜
Figure caption: Comparison of temperature gradients for the five 3D RHD models including the realized temperature gradient, ∇3D, radiative temperature gradient, ∇rad, adiabatic gradient, ∇ad, and the modified model adiabatic temperature gradient including P turb, ﹩{{\rm{\nabla }}}_{\mathrm{ad}}^{{\prime} }﹩ (colored solid, colored dashed, black dotted, and gray dotted–dashed lines respectively). The vertical dashed lines are the same as in Figure 2. The gray shaded regions denote convectively unstable regions as in Figure 3.
Paper: Periodic Radio Emission from the T8 Dwarf WISE J062309.94–045624.6
Authors: Kovi Rose, Joshua Pritchard, Tara Murphy, Manisha Caleb, Dougal Dobie, Laura Driessen, Stefan W. Duchesne, David L. Kaplan, Emil Lenc, Ziteng Wang
Figure caption: Left: Stokes V dynamic spectrum (0.9–1.5 GHz) from the MeerKAT observation. The lower panel shows the Stokes V lightcurve. We used 1 MHz frequency bins and 64 s time sampling bins. The lightcurve and the dynamic spectrum display periodic behavior with complex subpulse structure. We do not include the Stokes I dynamic spectrum or lightcurve as they are heavily affected by artifacts from bright off-axis emission. Horizontal gaps correspond to frequencies that were flagged due to radio frequency interference (RFI) and the vertical gap corresponds to a calibration scan. Right: Stokes I and Stokes V continuum detection images from the MeerKAT observation.
Paper: Periodic Radio Emission from the T8 Dwarf WISE J062309.94–045624.6
Authors: Kovi Rose, Joshua Pritchard, Tara Murphy, Manisha Caleb, Dougal Dobie, Laura Driessen, Stefan W. Duchesne, David L. Kaplan, Emil Lenc, Ziteng Wang
Figure caption: Left: Lomb–Scargle periodogram of the 270 s time-sampled Stokes I and Stokes V data from the ATCA MJD 59929 observation. We plot the Stokes I (black) and Stokes V (red) power levels corresponding to the 5% (dotted) and 1% (dotted–dashed) false alarm probabilities for reference (top). The lower panel shows the 165 s time-sampled Stokes I and Stokes V ATCA lightcurves phase folded to P = 1.89 hr. For both panels we use the lower 700 MHz of the ATCA observing band with 10 MHz frequency binning. Right: Lomb–Scargle periodogram of the 64 s time-sampled Stokes V data from the MeerKAT observation. We plot the Stokes V (red) power levels corresponding to the 0.1% (dotted–dashed) and 1% (dotted) false alarm probabilities for reference (top). The lower panel shows the 105 s time-sampled Stokes V MeerKAT lightcurves phase folded to P = 1.91 hr. For both panels we use the 0.9–1.5 GHz part of the MeerKAT observing band with 1 MHz frequency binning.
Paper: Periodic Radio Emission from the T8 Dwarf WISE J062309.94–045624.6
Authors: Kovi Rose, Joshua Pritchard, Tara Murphy, Manisha Caleb, Dougal Dobie, Laura Driessen, Stefan W. Duchesne, David L. Kaplan, Emil Lenc, Ziteng Wang
Figure caption: Left: Stokes V dynamic spectrum (1.3–2.0 GHz) from the MJD 59929 ATCA observation. The lower panel shows the Stokes V (red) and Stokes I (black) lightcurves. We used 10 MHz frequency bins and 270 s time sampling bins. Both lightcurves and the dynamic spectrum display a clear periodicity. We do not show the Stokes I dynamic spectrum as it is heavily affected by artifacts from bright off-axis emission. Horizontal gaps correspond to frequencies that were flagged due to radio frequency interference (RFI). Right: Stokes I and Stokes V continuum detection images from the MJD 59929 ATCA observation.
Paper: The First JWST Spectral Energy Distribution of a Y Dwarf
Authors: Samuel A. Beiler, Michael C. Cushing, J. Davy Kirkpatrick, Adam C. Schneider, Sagnick Mukherjee, Mark S. Marley
Figure caption: Three sections of interest from our spectrum (black), with important molecular cross sections plotted over top (color). These cross sections were calculated at P = 1 bar and T = 500 K. Note that the y-axis for the cross sections is inverted for clarity. Top: we tentatively identify a new NH3 absorption feature found at 3 μm. H2O and CH4 set the red and blue edges of this peak, but the strong Q branch of the ν 1 ammonia band carves out a small notch in the peak. Middle: the 5 μm peak is shaped by both CO and CO2 features. Both of these molecules are not expected in equilibrium models of ∼500 K, but are found in models that account for vertical mixing in the atmosphere. Bottom: from 8–12 μm ammonia is the dominant absorber in WISE 0359−54’s atmosphere. The ν 2 Q-branch doublet at 10.3 and 10.7 μm has been seen before, but the P and R branches of ammonia on either side are seen for the first time.
Paper: The First JWST Spectral Energy Distribution of a Y Dwarf
Authors: Samuel A. Beiler, Michael C. Cushing, J. Davy Kirkpatrick, Adam C. Schneider, Sagnick Mukherjee, Mark S. Marley
Figure caption: The first full spectral energy distribution (black) from 1–21 μm of a Y dwarf (WISE 0359−54), with key molecular features identified (color). It consists of merged and calibrated JWST spectra and photometry (F1500W, F1800W, and F2100W), in dimensions of f  ν . The transition between the NIRSpec and MIRI LRS spectra occurs at 5.14 μm and can be seen easily by the change in resolving power. The FWHM of the photometric bandpasses are marked with horizontal bars, while the vertical bars on the photometric points represent the 1σ flux density error. The typical signal-to-noise of the NIRSpec and MIRI LRS spectra are ∼20 and ∼100, respectively.(The data used to create this figure are available.)
Paper: The First JWST Spectral Energy Distribution of a Y Dwarf
Authors: Samuel A. Beiler, Michael C. Cushing, J. Davy Kirkpatrick, Adam C. Schneider, Sagnick Mukherjee, Mark S. Marley
Figure caption: The distributions of a million radii and effective temperatures for WISE 0359−54 drawn and calculated as described in Section 5, shown both as histograms and as box-and-whisker plots. The box-and-whisker plots divide the data into quartiles, with the median value marked as an orange line and the mean as a green triangle. We use luminosities drawn from a Gaussian distribution based on our calculated value along with ages drawn from a uniform 1–10 Gyr distribution to generate the radii distribution on the left. Each luminosity drawn and corresponding radius are used to calculate a T eff, resulting in the distribution on the right. For reference we include a zeroth-order approximation in the form of red lines at 1 ﹩{{ \mathcal R }}_{{\rm{J}}}^{{\rm{N}}}﹩ and ﹩{T}_{\mathrm{eff}}^{{R}_{{\rm{J}}}}﹩. The pileup at 1.04 ﹩{{ \mathcal R }}_{{\rm{J}}}^{{\rm{N}}}﹩ in the model radii distribution translates to the bump in the T eff distribution around 445 K.
Paper: The First JWST Spectral Energy Distribution of a Y Dwarf
Authors: Samuel A. Beiler, Michael C. Cushing, J. Davy Kirkpatrick, Adam C. Schneider, Sagnick Mukherjee, Mark S. Marley
Figure caption: Isochrones (gray) and cooling tracks (black) from the Sonora Bobcat evolutionary models in the effective temperature surface gravity plane. We plot the best-fit model at its log g and T eff (orange), as well as the loci of points consistent with the observed bolometric luminosity and an age range estimate (1–10 Gyr, blue), with the blue dashed lines indicating ±1σ. The best-fit model’s low surface gravity corresponds to an age of 20 Myr and a significantly lower mass of ∼1 M Jup, compared to the lowest value of ∼10 M Jup of our semiempirical range.
Paper: The First JWST Spectral Energy Distribution of a Y Dwarf
Authors: Samuel A. Beiler, Michael C. Cushing, J. Davy Kirkpatrick, Adam C. Schneider, Sagnick Mukherjee, Mark S. Marley
Figure caption: The best-fitting Sonora model and its simulated photometry (orange) for our observed spectrum and photometry (black) with wavelength in log space. Overall, the fit is good given the broad wavelength coverage of the observations, with the model having some difficulties matching the features at the 5 μm peak and an overprediction of flux past 11 μm. The effective temperature of the model is within 1σ to our calculated effective temperature.
Paper: The First JWST Spectral Energy Distribution of a Y Dwarf
Authors: Samuel A. Beiler, Michael C. Cushing, J. Davy Kirkpatrick, Adam C. Schneider, Sagnick Mukherjee, Mark S. Marley
Figure caption: The offset of the model spectrum’s fitted peaks and observed spectrum’s peaks as a function of the observed wavelength (black), with a linear fit that we used to correct the MIRI wavelength calibration.
Paper: An Observed Transition of Galaxy Spins on Void Surfaces
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Mean alignments between galaxy spins and directions toward the nearest void centers (purple filled circles) with bootstrap errors, along with ±1σ scatter among the 1000 randomly shuffled resamples (violet dotted lines). The main result is detection of the occurrence of the stellar spin transition of the spiral galaxies on void surfaces for the VoidFinder case.
Paper: An Observed Transition of Galaxy Spins on Void Surfaces
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Confidence levels (purple filled circles) at which the null hypothesis of no alignments is rejected by the KS one sample test, along with the ±1σ scatter among the 1000 randomly shuffled resamples (violet dotted lines). The main result is the constraint of the spin transition mass threshold to the range of ﹩9.51\leqslant \mathrm{log}\left[{M}_{\mathrm{th},\star }/(\,{h}^{-1}\,{M}_{\odot })\right]\leqslant 10.3﹩.
Paper: An Observed Transition of Galaxy Spins on Void Surfaces
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Schematic representation of two different realizations of the 3D spins of a spiral galaxy and the direction toward the nearest void center.
Paper: An Observed Transition of Galaxy Spins on Void Surfaces
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Same as Figure 2 but treating the Sab and Scd galaxies separately (red and blue filled circles, respectively), along with the 1σ scatter among the randomly shuffled resamples (pink and sky blue dotted lines). No signal of the occurrence of the stellar spin transition at a fixed morphological type.
Paper: An Observed Transition of Galaxy Spins on Void Surfaces
Authors: Jounghun Lee, Jun-Sung Moon
Figure caption: Same as Figure 4 but as a function of the bulge stellar mass. Disappearance of the spin transition signal at fixed morphology should not be due to the difference between the Sab and Scd galaxies in their bulge masses.
Paper: Jetted and Turbulent Stellar Deaths: New LVK-detectable Gravitational-wave Sources
Authors: Ore Gottlieb, Hiroki Nagakura, Alexander Tchekhovskoy, Priyamvada Natarajan, Enrico Ramirez-Ruiz, Sharan Banagiri, Jonatan Jacquemin-Ide, Nick Kaaz, Vicky Kalogera
Figure caption: 3D rendering of the cocoon-powered GW strain density in cgs units, as calculated in the lab frame without considering retarded time effects. The snapshots are when the cocoon breaks out from the star, 2.5 s after the BH formation—the width of panel (b) is ∼2R ⋆ = 8 × 1010 cm. At θ obs = 0° the cocoon projection appears nearly axisymmetric and results in a weak on-axis signal (a), whereas at larger observer angles the asymmetric shape of the cocoon leads to strong GW emission (b).
Paper: Jetted and Turbulent Stellar Deaths: New LVK-detectable Gravitational-wave Sources
Authors: Ore Gottlieb, Hiroki Nagakura, Alexander Tchekhovskoy, Priyamvada Natarajan, Enrico Ramirez-Ruiz, Sharan Banagiri, Jonatan Jacquemin-Ide, Nick Kaaz, Vicky Kalogera
Figure caption: The number of detectable GW events in CE (green) in 1 yr, A+ (blue+purple) in 2 yr, and O4 (pink+purple) in 1.5 yr as a function of the maximum isotropic equivalent γ-ray energy ﹩\,{E}_{\gamma ,\mathrm{iso},\max }﹩ (the cutoff of the power-law fit to N LGRBs(E  γ,iso) distribution), assuming MF S/N values, and a minimum S/N for detection of 20. These rates are calculated self-consistently with our simulation for wobbling jets. The range in the number of detectable events reflects the uncertainty in the jet opening angle. The detection rate of outflows with ﹩E\lt {E}_{\max }﹩ also indicates the abundance of LGRB events among SNe Ib/c (right vertical axis labels).
Paper: Jetted and Turbulent Stellar Deaths: New LVK-detectable Gravitational-wave Sources
Authors: Ore Gottlieb, Hiroki Nagakura, Alexander Tchekhovskoy, Priyamvada Natarajan, Enrico Ramirez-Ruiz, Sharan Banagiri, Jonatan Jacquemin-Ide, Nick Kaaz, Vicky Kalogera
Figure caption: Top: 3D rendering of off-axis (a) and on-axis (b) projections of the cocoon mass density after breakout from the star (star is in the center shown in white), taken from Gottlieb et al. (2022b). Middle: on- and off-axis strain amplitudes of a typical LGRB event, shown in the time (c) and frequency (d) domains. Bottom: normalized strain amplitude (by maximum off-axis amplitude) spectrograms for a sliding window of 100 ms, shown for off-axis (e) and on-axis (f) observers.
Paper: Jetted and Turbulent Stellar Deaths: New LVK-detectable Gravitational-wave Sources
Authors: Ore Gottlieb, Hiroki Nagakura, Alexander Tchekhovskoy, Priyamvada Natarajan, Enrico Ramirez-Ruiz, Sharan Banagiri, Jonatan Jacquemin-Ide, Nick Kaaz, Vicky Kalogera
Figure caption: Jets (light blue) inflate the hourglass-shaped cocoon (dark blue) inside of a dying massive star (pale yellow). The jets run into and shock against the collapsing star, forming backflows (yellow arrows). The in-falling star runs into and shocks against the backflows (red arrows). The shocked jets and shocked stellar components form the cocoon and turbulently mix inside of it (white arrows).
Paper: Turbulence-supported Massive Star Envelopes
Authors: William C. Schultz, Lars Bildsten, Yan-Fei Jiang, 燕飞 姜
Figure caption: HRD showing the five 3D models (colored points). Squares represent models from Jiang et al. (2018) while the stars denote models from Schultz et al. (2022) and this work. The error bars show the difference between definitions of T eff described in Section 3.1. The black lines are MESA models from Cantiello et al. (2021). The vertical dashed lines are approximate contours of τ Fe/τ crit as calculated from the MESA models. Gray shaded regions show the S Dor and luminous blue variable (LBV) outburst instability strips from Smith et al. (2004).
Paper: Turbulence-supported Massive Star Envelopes
Authors: William C. Schultz, Lars Bildsten, Yan-Fei Jiang, 燕飞 姜
Figure caption: Fractional difference from HB for the average pressure of 3D models vs. ﹩{{ \mathcal M }}_{{\rm{\Psi }}}﹩ including and excluding turbulent pressure (solid and dashed respectively). Vertical dashed lines on the right denote the location where the energy flux matches the photospheric criteria of σ T 4 (e.g., T = T eff,F  from Table 1).
Paper: ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274
Authors: Alexandra Pope, Jed McKinney, Patrick Kamieneski, Andrew Battisti, Itziar Aretxaga, Gabriel Brammer, Jose M. Diego, David H. Hughes, Erica Keller, Danilo Marchesini, Andrew Mizener, Alfredo Montaña, Eric Murphy, Katherine E. Whitaker, Grant Wilson, Min Yun
Figure caption: (Top left) Image plane showing the HST v-band image with the ALMA [C II] and dust continuum contours (3σ and 5σ). The corresponding ALMA beams are shown in the bottom right. Az9 is the multiple image source 5.2, and we rule out any millimeter emission coming from another nearby source, 12.2. The red dashed lines show the region we used for the HST source plane reconstruction. (Top right) Extracted 1D spectrum (from image plane cube) of Az9 (black) and best-fit Gaussian to the [C II] line (dashed blue line). (Bottom left) Source plane reconstructed images: HST H-band (λ rest = 0.3 μm) image with the ALMA [C II] and dust continuum contours (3σ and 5σ). The image cutout size is 1.″2 ×1.″2. The colored crosses denote the centroids of each image. The ALMA [C II] reconstructed beam is shown in the bottom right corner. (Bottom right) Source plane reconstructed [C II] moment 1 map with light and dark gray contours showing the HST and Band 6 dust continuum, respectively.
Paper: ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274
Authors: Alexandra Pope, Jed McKinney, Patrick Kamieneski, Andrew Battisti, Itziar Aretxaga, Gabriel Brammer, Jose M. Diego, David H. Hughes, Erica Keller, Danilo Marchesini, Andrew Mizener, Alfredo Montaña, Eric Murphy, Katherine E. Whitaker, Grant Wilson, Min Yun
Figure caption: Kinematics of [C II] in Az9 in the source plane image. The top panels show the line-of-sight rotational velocity, and the bottom panels show the velocity dispersion. In the top left panel, we plot both the model and data velocities extracted along the major axis over the empirical position-velocity (P-V) diagram (black histogram). Contours from the model P-V are shown in red, and uncertainties on the empirical P-V along the major axis are shown with a green line. The bottom left panel shows the velocity dispersion extracted along the major axis for the data, model, and uncertainties similar to the top left panel. Moment maps from the reconstructed cube are shown in the data column, followed by maps from the tilted ring model and the residual between the two. The global fit strongly favors a rotating disk with a maximum rotational velocity of 139 km s−1 and dispersion of 26 km s−1 and reproduces the line-of-sight velocity map along the major axis remarkably well (top left panel). The reconstructed beam is shown in gray.
Paper: ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274
Authors: Alexandra Pope, Jed McKinney, Patrick Kamieneski, Andrew Battisti, Itziar Aretxaga, Gabriel Brammer, Jose M. Diego, David H. Hughes, Erica Keller, Danilo Marchesini, Andrew Mizener, Alfredo Montaña, Eric Murphy, Katherine E. Whitaker, Grant Wilson, Min Yun
Figure caption: (Top) SED of Az9 (red symbols) with the best-fit model from MAGPHYS_highz (black open circles and curve). Data with S/N < 3 are treated as 3σ upper limits (red arrows). The colored curves show the best-fit model excluding the ALMA data (green) and excluding the ALMA, F555W, F606W, and F625W data (orange). Interestingly, the F555W, F606W, and F625W bands, which cover the range between the Lyman limit and the Lyα line, appear to place strong constraints on the dust emission. (Bottom) Histograms showing the best-fit values for stellar mass, SFR, sSFR, and dust luminosity for the three models shown in the top panel. The median values and uncertainties (from the 16th and 84th percentiles) for each property from the best-fit model to all bands (black) are shown in the top right corner of each panel. The derived parameters are consistent for the fits with and without the ALMA data.
Paper: ALMA Reveals a Stable Rotating Gas Disk in a Paradoxical Low-mass, Ultradusty Galaxy at z = 4.274
Authors: Alexandra Pope, Jed McKinney, Patrick Kamieneski, Andrew Battisti, Itziar Aretxaga, Gabriel Brammer, Jose M. Diego, David H. Hughes, Erica Keller, Danilo Marchesini, Andrew Mizener, Alfredo Montaña, Eric Murphy, Katherine E. Whitaker, Grant Wilson, Min Yun
Figure caption: (Left) Total SFR as a function of stellar mass for galaxies at z ∼ 4–5. The gray shaded region shows ±1σ from the galaxy main sequence at z = 4.5 from Speagle et al. (2014). In both panels, Az9 is shown as a red star. The blue filled triangles are individual galaxies from ALPINE that are detected in the dust continuum. (Right) Fraction of star formation that is obscured by dust (f obscured) as a function of the stellar mass. Open triangles show the stacked measurements for the ALPINE sample, which are lower in f obscured than the subset of sources detected in the dust continuum (filled triangles). The green curve is the best-fit relation for z = 0–2.5 from Whitaker et al. (2017), while the blue dashed curve is the same function scaled down (a = 6 × 109 and b = −2.284 following Equation (1) of Whitaker et al. 2017) to fit the ALPINE stacked measurements.