adsabs/AstroCLIMB huggingface dataset:
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Observed and modeled SEDs for a representative sample of our UFOs with the observed JWST photometry as black points, observed HST/Spitzer photometry as gray points, model photometry as red points, and the model spectrum in red. Photometric points with negative fluxes are indicated with the gray arrows. The SEDs in each column show the lowest (top SED) and highest (bottom SED) value galaxy in terms of stellar mass (left), sSFR (middle), and diffuse dust A  V  (right). We note that some of the SED fits are not ideal, particularly for the HST/Spitzer photometry of the galaxies in the left column. However, fits like these are not representative of the majority of our sample, and we also find that the stellar population parameter inferences are not strongly changed if only JWST photometry is used, so we keep these objects in our analysis.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Color images (F200W, F277W, F444W) of 35 of our UFOs illustrating the extended red nature of these objects. Identifiers in the upper left are the IDs in the JADES photometric catalogs and a 1″ bar is shown for reference in the lower right. These 1″ scale bars translate to physical sizes of 6.7–8.5 kpc depending on the redshift of the object. For comparison, we show a “typical” galaxy in the upper left panel with bluer colors and more pronounced color variations than the UFOs.
Paper: Braving the Storm: Quantifying Disk-wide Ionized Outflows in the Large Magellanic Cloud with ULLYSES
Authors: Yong Zheng, 永 郑, Kirill Tchernyshyov, Knut Olsen, Yumi Choi, Chad Bustard, Julia Roman-Duval, Robert Zhu, Enrico M. Di Teodoro, Jessica Werk, Mary Putman, Anna F. McLeod, Yakov Faerman, Raymond C. Simons, Joshua Peek
Figure caption: 2D velocity distributions of HVC90-175 in the same orthographic projection as in Figure 11. In the left panel, we find that the O I gas, as measured by Lehner et al. (2009), is moving faster at v LSR ∼ 150–175 km s−1 toward the west. Meanwhile, S II (middle), Si IV (not shown), and C IV (right) show nearly constant v LSR at ∼120 km s−1 across the surface of the cloud.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: F200W − F444W color vs. the semimajor axis effective size illustrating our optically faint galaxy color selection and our UFO size cut (dashed black line at 0.″25).
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Comparison between the HST color image (F606W, F125W, F160W) and the JWST color image (F200W, F277W, F444W) for a representative sample of our UFOs. As can be seen, these galaxies are very bright and prominent with JWST imaging, but almost or completely invisible at HST wavelengths.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: From left to right, we show how the UFOs, smaller OFGs, and bluer F444W-parent samples are distributed in the planes of size–mass, Sérsic index−mass, Sérsic index−size, and axis ratio−size. The histograms for the OFGs include the contribution from UFOs and the F444W-parent histograms include all galaxies in our samples. The solid black lines in the size–mass panel show the size–mass relationships from Suess et al. (2019a), demonstrating that UFOs generally lie on or slightly above the star-forming relation while the OFGs are scattered around the quiescent size–mass relation (which is largely a result of our size cut). From the other two panels, we can see that the optically faint galaxies have a much higher density of n < 2 objects, particularly for UFOs, relative to the bluer F444W-parent sample. There are no strong trends between the Sérsic index and stellar mass or effective size. The rightmost panel shows q vs. r  e  illustrating that optically faint galaxies have a range of sizes and tend to have lower q values (especially for the UFOs).
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Summary of the results from our axis-ratio modeling with the BEAST. The top row shows the observed axis-ratio distributions in black compared with the best-fitting (maximum a posteriori) model distributions in red. Lighter red lines show q distributions for random draws of the posterior distributions of μ  E , μ  T , σ  E , σ  T . The middle row shows random draws from the best-fitting model distribution in the intrinsic axis-ratio space, illustrating how the four distinct regions are defined and what the contribution from each region is. In the bottom row, we show the predicted fractions of four different galaxy shapes: elongated/prolate (blue), spheroidal (green), thick disk (purple), and thin disk (red). From left to right, we show the fully free version of the axis-ratio model, the model with restricted inclination, and the model with restricted inclination and a stronger preference for oblate galaxies. Here, vertical lines are the best-fit value for the fraction, horizontal lines show the 68% confidence interval, and the violin plots (shaded areas) give a representation of the distribution with wider regions having more probability.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Left panel: stellar mass inferred from SED fitting vs. redshift inferred from EaZY with UFOs in red, smaller optically faint galaxies in black, the bluer F444W-selected sample in gray, and ultrared SMGs from Ma et al. (2019) in purple. Right panel: how our objects are distributed in SFR and ﹩\mathrm{log}(M/{M}_{\odot })﹩ with the shaded gray region showing the SFMS at z = 2.5 from Leja et al. (2022). The UFOs are a much less extreme population than the optically faint FIR-selected galaxies, with lower stellar masses and SFRs. They occupy the high-mass end of all F444W-selected galaxies showing that it is not only extreme starbursts that were missed in previous censuses but also more moderate galaxies.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: How the inferred stellar population parameters and predicted spectra of the UFOs compare between their inner regions (0.″3 circular aperture) and outer regions (0.″6–0.″3 annulus). Top panels: from left to right we show the ratio or difference between the inner and outer stellar mass, A  V , MWA, and sSFR as a function of the stellar mass inferred from the integrated fits discussed in Section 3. The red and gray dashed lines show the median value of the ratio and where the values are equal. The red stripe shows the ∼1σ spread in the ratio or difference. Bottom panel: median posterior spectra for the inner and outer regions generated from the maximum probability samples of the individual objects showing that the inner and outer median UFO spectra are most similar at redder wavelengths.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Left: MWA vs. dust attenuation for the UFOs (red), smaller optically faint galaxies (black), and the bluer F444W-selected galaxies in gray. The optically faint galaxies have larger dust attenuations than the bluer comparison sample, but similar MWAs suggest that the redness of the optically faint galaxies is largely driven by elevated dust attenuation. Right: stellar mass vs. dust attenuation for the same samples along with the values inferred for the inner and outer regions of the UFOs as described in Section 4.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Left panel: observed UFO axis-ratio distribution (black) compared with different q distributions generated for different mock galaxy populations (prolate/blue, thick disk/solid orange, thin disk/dashed orange) showing the plausible galaxy types that could give rise to the observed q UFO distribution. Right panel: same as the left panel, but for different linear combinations of distinct populations (inclined thick/thin disks in orange, prolate/thin disk in blue, and prolate/inclined thin disk in purple). It is difficult to reproduce q UFO without both an inclined thin-disk population and a prolate population.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Observed colors vs. observed AB magnitude in F444W for our optically faint galaxies and the bluer, mass- and redshift-matched, F444W-selected sample. For the UFOs, we show the color in the inner 0.″3 circular aperture (filled red circles) as well as in an outer annulus of width 0.″3 (open red circles). The optically faint galaxies are clearly much redder than the parent sample with UFOs being consistently red throughout with red colors in their inner and outer regions.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Axis-ratio distributions for the UFOs and the entire sample of galaxies considered in this work split into low-mass (M * < 1010.4 M ⊙) and high-mass (M * < 1010.4 M ⊙) samples. It can clearly be seen that the majority of the low q objects in our whole sample are predominately coming from lower-mass UFOs but with a strong contribution from the higher-mass UFOs as well. The q distribution of low-mass UFOs is largely consistent with a prolate population, but the lower sample size of the high-mass group makes it harder to come to strong conclusions about the intrinsic shapes of the higher-mass UFOs.
Paper: JADES Ultrared Flattened Objects: Morphologies and Spatial Gradients in Color and Stellar Populations
Authors: Justus L. Gibson, Erica Nelson, Christina C. Williams, Sedona H. Price, Katherine E. Whitaker, Katherine A. Suess, Anna de Graaff, Benjamin D. Johnson, Andrew J. Bunker, William M. Baker, Rachana Bhatawdekar, Kristan Boyett, Stephane Charlot, Emma Curtis-Lake, Daniel J. Eisenstein, Kevin Hainline, Ryan Hausen, Roberto Maiolino, George Rieke, Marcia Rieke, Brant Robertson, Sandro Tacchella, Chris Willott
Figure caption: Axis-ratio distributions for the full F444W-parent sample, the optically faint sample, and the subset of UFOs. Compared to the other distributions, the UFO distribution is much more skewed toward lower values of q with the bulk of UFOs having q < 0.4. The other OFGs tend to have a fairly large number of low q objects as well but also have more q > 0.5 objects similar to what is seen in the full-parent sample.
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: All the bursts detected by VLA/realfast and GBT. The top panel shows the frequency-averaged, dedispersed time series of each bursts, and the bottom panel shows the frequency–time spectrum of the dedispersed bursts. The realfast bursts are dedispersed at the average DM = 1015.6 pc cm−3. The realfast data have a time resolution of 10 ms and are downsampled to a frequency resolution of 2 MHz. All GBT bursts are dedispersed at the average DM per epoch (ref. 3.1). The GBT burst data are downsampled to a time resolution of 1.95 ms and the frequency resolution of 1.95 MHz in the L band and 23.42 MHz in the C band.
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: Transient phase space. The black triangles shows bursts from J1818–1531. The downward triangles represent the full pulse sample, and the upward triangle represents the subpulse sample. The darker and lighter shades of the triangles represent the luminosities using NE2001 and YMW16, respectively. This figure is adapted from Nimmo et al. (2022).
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: Normalized polarization profiles and PA for GBT bursts. The red and blue dashed lines indicate linear and circular polarization, respectively. The top panel shows PA curves fitted with 1σ error bars. The burst names are also indicated.
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: The frequency dependence of scattering timescales for bursts in Epoch 1 and 2 L-band observations. Burst L4 (in blue) from Epoch 1 and burst L6 (in orange) from Epoch 2 is plotted and their best-fitting curve is marked by dashed lines of respective colors. See Section 4.3 for more details about the plot.
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: The burst fluxes as a function of frequency. The dots shows the flux in Jy. The error bar measurement is described in Section 4.2. The gray line shows the best-fit slope to all data points as described in Section 4.2.
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: The profile of GBT bursts fitted by Gaussian convolved with exponential tail model. Some bursts are a sum of multiple Gaussian exponentials. The orange solid line shows the fit to the profile, and the dotted orange lines show the fitted components. The multiple components contribute to the subpulse sample. The fitting residuals are shown in the bottom panel of each plot.
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: The dirty image (on the top panel) and clean image (on the bottom panel) of the realfast bursts at 1.4 GHz. We have not used R4 and R5 for the positional analysis. The synthesized beam is shown in the lower left corner.
Paper: An Unidentified Fermi Source Emitting Radio Bursts in the Galactic Bulge
Authors: Reshma Anna-Thomas, Sarah Burke-Spolaor, Casey J. Law, F. K. Schinzel, Kshitij Aggarwal, Geoffrey C. Bower, Liam Connor, Paul B. Demorest
Figure caption: Here, we display the relative layout of field sources and error regions. The main image shows the deep VLA observation in grayscale. The large yellow and small dark blue ellipses represent the 3FGL and 4FGL Fermi detections, respectively. The orange marker represents the realfast localization. The light pink markers in the northern and southern edge of the image are unrelated pulsars. The black contours show 330 MHz emission in the region from Brogan et al. (2006) at levels at 9 mJy × 2 n , where n = (0, 1, 2, ...). The red diamond represents the HESS source, presumed PWN, associated with the supernova shown. The inset image shows the average realfast R.A./decl. errors represented as an ellipse (orange) on the grayscale PAN-STARRS i-band image, with the dotted blue circle representing the location and a nominal 0.″5 R.A./decl. error radius of PSO J274.6436-15.5258 as identified by GAIA (see Section 5.1). The magenta ellipse to the southeast represents the position and error radius of the X-ray source identified by XMM-Newton.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: Top panel: the height–time plot of slit 122, with its three color-coded and numbered clicked positions shown as stars. The middle row shows the cutout images centered on each respective point ±20 pixels and the point of each maximum intensity shown as a diamond along each perpendicular white line. Bottom row: the corresponding intensity plots with the star (clicked image position from upper panel), diamond (the automatically determined peak intensity location along the diagonal image slit from the middle row), and the manually chosen position of the knot half-width as a triangle.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: As Figure 4, but for slit 260 and points 2, 10, and 17, respectively.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: The instantaneous image of the FOV at the Hα line core. Each white line shows the location of every 20th slit of those used here. The red slits correspond to slits 122 and 260, which will be used as examples.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: The simulated mass density ρ, at 400 s in the x–z plane for all runs across the parameters. The critical wavelength λ  c  is displayed along the figure’s y-axis, and the initial magnetic field strength B 0 along the figure’s x-axis. The horizontal solid blue lines labeled 1–6 represent the three slits used to determine knot widths for a coincident knot seen in all simulations, here selected over a range of B 0. The horizontal solid yellow lines labeled (a)–(c) represent three slits used to determine knot intensity ratios and the z-component of velocity, over the range of λ  c . The yellow box represents a space within the parameter ranges that we identify as being the best at characterizing most of the observable properties for the majority of knots observed with the SST.
Paper: The Observational and Numerical Analysis of the Rayleigh–Taylor Instability beneath a Hedgerow Prominence
Authors: T. Rees-Crockford, E. Scullion, E. Khomenko, Ángel de Vicente
Figure caption: (a) The instaneous radial plane-of-sky velocity, v  z , distribution of the 856 pairs of points. (b) The distribution of plane of sky velocity vs. averaged knot height above limb.