adsabs/AstroCLIMB huggingface dataset:
Paper: Atomic Gas Scaling Relations of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The redshift distributions of the three sSFR subsamples. The blue histograms show, for each sSFR subsample, the number (N) of HI 21 cm subcubes normalized by the total number of subcubes in the corresponding subsample, for the different redshift intervals. The HI 21 cm subcubes of each sSFR subsample were assigned weights such that each effective redshift distribution is identical to the redshift distribution of the low-sSFR subsample (orange lines). The total number of galaxies in the subsample is indicated in each panel, with the number of HI 21 cm subcubes shown in parentheses.
Paper: Atomic Gas Scaling Relations of Star-forming Galaxies at z ≈ 1
Authors: Aditya Chowdhury, Nissim Kanekar, Jayaram N. Chengalur
Figure caption: The redshift distributions of the three stellar-mass subsamples. The blue histograms show, for each stellar-mass subsample, the number of HI 21 cm subcubes in different redshift intervals (N), obtained after normalizing by the total number of subcubes in the corresponding subsample. The HI 21 cm subcubes of each stellar-mass subsample were assigned weights such that each effective redshift distribution is identical to the redshift distribution of the low-stellar-mass subsample (orange lines). The number of galaxies in the subsample is indicated in each panel, with the number of HI 21 cm subcubes shown in parentheses.
Paper: A Localized Kinematic Structure Detected in Atomic Carbon Emission Spatially Coincident with a Proposed Protoplanet in the HD 163296 Disk
Authors: Felipe Alarcón, Edwin A. Bergin, Richard Teague
Figure caption: Velocity-centroid map of the C I 3P1-3P0 line emission using bettermoments with a Gaussian fit. Overlaid are the contours of the 13CO J = 2−1 centroid map from the MAPS data (Law et al. 2021) at 0.″15 resolution. We show the region of the deepest gap in HD 163296 with dashed lines and the minor axis of the disk with a black line. The figure shows that the C I line emission has a strong redshifted component, ∼2 km s−1 velocity offset, located at ∼0.″5 to the SW of the star, while the 13CO velocity-centroid contours show a Keplerian profile. The synthesized beam is shown on the left corner of the figure. It is noteworthy that the deepest dust continuum gap of the HD 163296 disk is located at that radius (Isella et al. 2018).
Paper: A Localized Kinematic Structure Detected in Atomic Carbon Emission Spatially Coincident with a Proposed Protoplanet in the HD 163296 Disk
Authors: Felipe Alarcón, Edwin A. Bergin, Richard Teague
Figure caption: C I abundance in a thermochemical model of HD 163296, including the gaps and ring from dust continuum emission (Isella et al. 2018) run with rac2d (Du et al. 2014). Contours are drawn for the CO abundance in the disk. The figure shows that inside the gap at 48 au, particularly toward the outer edge, the C I abundance increases toward the midplane due to the transparency to UV in that region. Thus, it is possible that C I line emission can trace vertical protoplanet infall in the disk.
Paper: A Localized Kinematic Structure Detected in Atomic Carbon Emission Spatially Coincident with a Proposed Protoplanet in the HD 163296 Disk
Authors: Felipe Alarcón, Edwin A. Bergin, Richard Teague
Figure caption: Kinematic deviations between the velocity-centroid map of the C I 3P1-3P0 line emission and the CO J = 2−1 line from the MAPS survey (Öberg et al. 2021) at matching spectral and spatial resolutions. The background is showing the DSHARP 1.3 mm dust continuum emission of the HD 163296 disk clipped at 65 μJy beam−1 (Andrews et al. 2018). The CO J = 2−1 velocity centroid was used as a proxy for the Keplerian rotational profile of the disk to isolate the kinematic anomaly observed in C I. The figure shows a bipolar flow centered at the 48 au gap and at the same azimuthal location as the putative planet proposed by Isella et al. (2018). The synthesized beam is shown on the left corner of the figure.
Paper: A Localized Kinematic Structure Detected in Atomic Carbon Emission Spatially Coincident with a Proposed Protoplanet in the HD 163296 Disk
Authors: Felipe Alarcón, Edwin A. Bergin, Richard Teague
Figure caption: Integrated spectra of the CO J = 2−1 and the C I 3P1-3P0 line emission integrated over a 60° wedge, 60 au long, centered at 48 au on the SW orientation of the minor axis of the disk. The dim, dashed lines show the respective noise levels of each integrated spectrum. Given that the integrated spectrum is centered on the minor axis, a Keplerian disk should produce a symmetric structure around the stellar velocity, such as the CO J = 2−1 emission, while the C I line emission has an important redshifted component located in the deepest dust gap of HD 163296 at 48 au. We mirrored the blueshifted C I emission with a dotted line to emphasize the redshifted emission excess in the wedge.
Paper: A Localized Kinematic Structure Detected in Atomic Carbon Emission Spatially Coincident with a Proposed Protoplanet in the HD 163296 Disk
Authors: Felipe Alarcón, Edwin A. Bergin, Richard Teague
Figure caption: CO self-shielding for the HD 163296 disk model with a dust-depleted gap at 48 au. CO self-shields itself even inside the gap. However, the content depletion inside the gap allows C I formation through CO destruction at the deeper layer. The model shows that CO self-shields ∼99% of the CO photodissociation photons 10 au above the midplane at 48 au.
Paper: A Localized Kinematic Structure Detected in Atomic Carbon Emission Spatially Coincident with a Proposed Protoplanet in the HD 163296 Disk
Authors: Felipe Alarcón, Edwin A. Bergin, Richard Teague
Figure caption: Velocity-centroid map of the C I 3P1-3P0 line for the 2013.1.00527.S and 2015.1.01137.S. data sets on the left and right, respectively. The kinematic feature in the SW of the disk is observed in both data sets independently.
Paper: Neutrinos from the Brightest Gamma-Ray Burst?
Authors: Kohta Murase, Mainak Mukhopadhyay, Ali Kheirandish, Shigeo S. Kimura, Ke Fang
Figure caption: (Left) Constraints on Γ as a function of r diss for different values of the CR loading factor ξ cr. The region below r ph is not considered for nonthermal neutrino production. (Middle) Constraints on ξ cr as a function of r diss for a given Lorentz factor of Γ = 102.5. (Right) Constraints on ξ cr as a function of Γ in the internal shock model, where the IceCube stacking limit at 90% C.L. (Aartsen et al. 2017a) is also shown. Note that color scale represents the number of signal events ﹩{{ \mathcal N }}_{{\rm{s}}{\rm{i}}{\rm{g}}}.﹩
Paper: Neutrinos from the Brightest Gamma-Ray Burst?
Authors: Kohta Murase, Mainak Mukhopadhyay, Ali Kheirandish, Shigeo S. Kimura, Ke Fang
Figure caption: Left) Energy fluences of quasi-thermal ν  μ  from GRB 221009A for both collision and decoupling scenarios, where ξ  N  = 5 and ﹩{{ \mathcal E }}_{\gamma }^{\mathrm{iso}}={10}^{54.5}﹩ erg are used. (Right) Expected number of signal events, ﹩{{ \mathcal N }}_{\mathrm{sig}}﹩, in DeepCore+IceCube as a function of ξ  N  and Γ. The solid and dashed lines show the parameter sets that lead to doublet and triplet events, respectively.
Paper: Polytropic Behavior in the Structures of Interplanetary Coronal Mass Ejections
Authors: M. A. Dayeh, G. Livadiotis
Figure caption: Time series of plasma parameters showing an ICME and the four examined regions highlighted as pre-ICME (pink), sheath (light brown), magnetic obstacle (green), and post-ICME (purple). (a) Proton speed, (b) Magnetic field components, (c) magnetic field magnitude, (d) proton number density, and (e) proton thermal speed.
Paper: Formation of Lunar Basins from Impacts of Leftover Planetesimals
Authors: David Nesvorný, Fernando V. Roig, David Vokrouhlický, William F. Bottke, Simone Marchi, Alessandro Morbidelli, Rogerio Deienno
Figure caption: Early impacts of diameter d > 20 km planetesimals on the Moon match the number of known lunar basins—on the assumption that the basin record started at t ≃ 190 Myr. The plot shows the accumulated number of impacts after time t, where t = 0 is the birth of the solar system, and t ≃ 4.57 Gyr is the present time. The profiles have a declining trend as younger surfaces accumulate fewer impacts. The planetesimal, asteroid, and comet profiles are shown by red, green, and blue lines, respectively; the black line is the total impact flux. The vertical dashed–dotted lines show the lower bound on the Moon-forming impact (t ∼ 30 Myr), estimated start of the lunar basin record (t ≃ 190 Myr or T ≃ 4.38 Ga), Imbrium formation (t ≃ 650 Myr or T ≃ 3.92 Ga), and transition from the planetesimal-dominated to asteroid-dominated impact stages (t ≃ 1.1 Gyr or T ≃ 3.5 Ga). The inset shows some of the lunar near-side basins.
Paper: Formation of Lunar Basins from Impacts of Leftover Planetesimals
Authors: David Nesvorný, Fernando V. Roig, David Vokrouhlický, William F. Bottke, Simone Marchi, Alessandro Morbidelli, Rogerio Deienno
Figure caption: The model impact chronology satisfies Imbrium-era constraints. The rainbow plot shows the normalized probability for Imbrium to form late (600 < t < 900 Myr, d > 100 km) and have exactly two basins (Orientale and Schrödinger, d > 20 km impactors) younger than Imbrium. We fix α = 0.45, and test different chronologies by varying the e-fold τ and relative calibration factor C r, where C r = 1 corresponds to the standard calibration of leftover planetesimals (Section 2.1). We generate a statistically large number of random impact sequences (∼105) for each pair (C  r , τ) and evaluate the likelihood of satisfying the condition described above. The likelihood is low if C  r  and/or τ are small, because it is difficult to form Imbrium. It is low if C  r  and/or τ are large, because more than one Imbrium forms and/or many smaller basins form after Imbrium. The star symbol denotes C r = 1 and τ = 6 Myr obtained from a fit to our simulation of leftover planetesimals.
Paper: Formation of Lunar Basins from Impacts of Leftover Planetesimals
Authors: David Nesvorný, Fernando V. Roig, David Vokrouhlický, William F. Bottke, Simone Marchi, Alessandro Morbidelli, Rogerio Deienno
Figure caption: Our model N 1 chronology matches crater counts on lunar terrains with known radiometric ages. The bold solid line is ﹩{N}_{1}{(T)=a\exp [-(t/\tau )}^{\alpha }]+{cT}﹩ with t = 4570 − T (t and T in Myr), a = 94 km−2, τ = 6 Myr, α = 0.45, and c = 10−6 km−2 Myr−1; the shaded area indicates the model uncertainty. The green (Neukum et al. 2001), red (Marchi et al. 2009), and blue dots (Robbins 2014) with associated error bars show different D > 1 km crater counts. The impact model also implies ≃25 D > 20 km craters per 106 km2 for T = 3.92 Ga, in a close match to N 20 = 26 ± 5 reported for the Fra Mauro/Imbrium highlands (Orgel et al. 2018). The Nectaris basin with N 20 ≃ 170 is estimated here to be T = 4.21–4.29 Gyr old.
Paper: Formation of Lunar Basins from Impacts of Leftover Planetesimals
Authors: David Nesvorný, Fernando V. Roig, David Vokrouhlický, William F. Bottke, Simone Marchi, Alessandro Morbidelli, Rogerio Deienno
Figure caption: Model impacts of diameter d > 10 km bodies on the Earth match the number of Archean spherule beds. The vertical dashed–dotted lines outline the late Archean period, T = 2.5–3.5 Ga, where the model predicts ≃20 d > 10 km impacts on the Earth. The sixteen known Archean spherule beds occur in two distinct time intervals, 2.4–2.7 Ga and 3.2–3.5 Ga (Marchi et al. 2021). If this is indicative of the average flux in the late Archean, there should be ∼14 additional spherule beds at 2.7–3.2 Ga. If so, the number of d > 10 km impacts in the model would represent ∼60% of the total number of spherule beds. For reference, some ∼43 d > 7 km impacts on the Earth are expected in the model at 2.5–3.5 Ga. The inset shows the Monteville spherule layer in South Africa (Reimold & Koeberl 2014).
Paper: Polytropic Behavior in the Structures of Interplanetary Coronal Mass Ejections
Authors: M. A. Dayeh, G. Livadiotis
Figure caption: (a) Illustration of the solar wind selection when calculating the polytropic index (see text for details). (b) Temperature vs. density plotted on a log-log scale, where the polytropic index is given as slope = γ-1. (c) Derived polytropic indices are plotted against the solar wind speed in a two-dimensional histogram. This spectrogram is normalized to the number of solar wind velocity bins (see Livadiotis & Desai 2016). The distribution of the polytropic indices is shown on the right.
Paper: Polytropic Behavior in the Structures of Interplanetary Coronal Mass Ejections
Authors: M. A. Dayeh, G. Livadiotis
Figure caption: (a) Histograms of all the events (green), of the selected events (yellow), and of the enriched data set of the good events (purple); modes are indicated and histograms are plotted for each region. (b) Calculated “jumps” of the polytropic modes and entropic gradients for R=1 au according to Equation (6).
Paper: New Constraints on the Dark Matter Density Profiles of Dwarf Galaxies from Proper Motions of Globular Cluster Streams
Authors: Khyati Malhan, Monica Valluri, Katherine Freese, Rodrigo A. Ibata
Figure caption: Using ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩ of GC streams to probe the DM density profiles inside their parent subhalos (or parent dwarf galaxies). Upper panel: each red/black/gray point represents the tangential velocity dispersion (﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩) of a particular simulated stream, and the corresponding error bar reflects the dispersion in the ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩ measurement along that stream. The y-axis denotes different simulations. The red points correspond to the in situ GC stream models and the black/gray points correspond to streams that accreted inside cuspy/cored subhalos (where small/large markers correspond to cases where subhalos had mass of M  =  108 M ⊙/109 M ⊙). The colored triangles are ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩ values we measure for five Milky Way streams, using Gaia EDR3 data. Lower panel: red/black/gray Gaussians correspond respectively to the distribution of simulated ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩ values from the in situ/cuspy/cored scenarios (including the scatter in the ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩ measurements). Gaussians with thin/thick borders correspond to cases where subhalos had mass of M = 108 M ⊙/109 M ⊙). In summary, in situ GC streams (red stars) possess extremely low values of ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩, GC streams accreted inside cuspy CDM subhalos (black diamonds) possess very large values of ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩, while streams accreted inside cored subhalos (gray circles) lie in between.
Paper: New Constraints on the Dark Matter Density Profiles of Dwarf Galaxies from Proper Motions of Globular Cluster Streams
Authors: Khyati Malhan, Monica Valluri, Katherine Freese, Rodrigo A. Ibata
Figure caption: Computing tangential velocity dispersion (﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩) of the Milky Way streams using Gaia EDR3. In a given column of this plot, all the panels provide details of a particular stream (the name of the stream is provided in the top panel). In a given column, panel (a) shows positions of the stream stars in the rotated (ϕ 1, ϕ 2) coordinate system, panel (b) shows the distance fit to the stream obtained using Gaia EDR3 parallaxes and photometry (where the fitted curves represent 100 Monte Carlo representations), and panel (c) shows the ﹩{v}_{\mathrm{Tan}}﹩ fit to the stream (where “﹩{v}_{\mathrm{Tan}}﹩ (obs)” is obtained by multiplying distance solutions of panel (b) with the Gaia EDR3 proper motion of stars. Panel (d) shows the residuals of the ﹩{v}_{\mathrm{Tan}}﹩ (obs) after the mean trend has been subtracted off, and the “blue band” represents the intrinsic dispersion. In panel (d), the quoted ﹩{\sigma }_{{v}_{\mathrm{Tan}}}﹩ value represents the median and the corresponding uncertainties reflect the 16th to 84th percentile range of the distribution (see text). Specifically for “GD-1,” we compare our distance fit with that of its orbit solution, only to ensure that our distance solutions are reliable (the orbit solution is taken from Malhan & Ibata 2019).
Paper: New Constraints on the Dark Matter Density Profiles of Dwarf Galaxies from Proper Motions of Globular Cluster Streams
Authors: Khyati Malhan, Monica Valluri, Katherine Freese, Rodrigo A. Ibata
Figure caption: Color–magnitude diagrams (CMDs) for five observed stellar streams (as indicated by labels) constructed from Gaia photometry. In each panel the observed, extinction corrected CMD (left, red points) and distance-corrected CMD (right, blue points) are shown. The knn values in the legend of each panel estimate the scatter in each CMD (smaller knn values imply less scatter).
Paper: New Constraints on the Dark Matter Density Profiles of Dwarf Galaxies from Proper Motions of Globular Cluster Streams
Authors: Khyati Malhan, Monica Valluri, Katherine Freese, Rodrigo A. Ibata
Figure caption: Same as Figure 2, but for different streams.
Paper: New Constraints on the Dark Matter Density Profiles of Dwarf Galaxies from Proper Motions of Globular Cluster Streams
Authors: Khyati Malhan, Monica Valluri, Katherine Freese, Rodrigo A. Ibata
Figure caption: Comparing our fitted d ⊙ and ﹩{v}_{\mathrm{Tan}}﹩ solutions with those obtained from Bailer-Jones et al. (2021) and Gaia EDR3. This plot corresponds to the “GD-1” stream.
Paper: PHANGS-JWST First Results: Spurring on Star Formation: JWST Reveals Localized Star Formation in a Spiral Arm Spur of NGC 628
Authors: Thomas G. Williams, Jiayi Sun, Ashley T. Barnes, Eva Schinnerer, Jonathan D. Henshaw, Sharon E. Meidt, Miguel Querejeta, Elizabeth J. Watkins, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Mélanie Chevance, Oleg V. Egorov, Eric Emsellem, Simon C. O. Glover, Kathryn Grasha, Hamid Hassani, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Ismael Pessa, Jérôme Pety, Francesca Pinna, Erik Rosolowsky, Karin M. Sandstrom, Rowan Smith, Mattia C. Sormani, Sophia Stuber, David A. Thilker, Bradley C. Whitmore
Figure caption: Three-color image of NGC 628, with ALMA CO in blue, MUSE Hα in green, and JWST 21 μm in red. The blue, red, and green boxes show the extent of each corresponding observation. The two spurs we focus on are shown as cyan (CO-rich), and orange (CO-poor) contours (see Section 3). Also shown are the spiral arms from the environmental mask, in gray. The position angle (21°; corresponding to θ = 0° in Figure 3) is indicated in the lower right, and a 1 kpc scalebar is shown in the lower left.
Paper: PHANGS-JWST First Results: Spurring on Star Formation: JWST Reveals Localized Star Formation in a Spiral Arm Spur of NGC 628
Authors: Thomas G. Williams, Jiayi Sun, Ashley T. Barnes, Eva Schinnerer, Jonathan D. Henshaw, Sharon E. Meidt, Miguel Querejeta, Elizabeth J. Watkins, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Mélanie Chevance, Oleg V. Egorov, Eric Emsellem, Simon C. O. Glover, Kathryn Grasha, Hamid Hassani, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Ismael Pessa, Jérôme Pety, Francesca Pinna, Erik Rosolowsky, Karin M. Sandstrom, Rowan Smith, Mattia C. Sormani, Sophia Stuber, David A. Thilker, Bradley C. Whitmore
Figure caption: A holistic overview of the spurs analyzed in this study. Left: three-color image of NGC628 produced from the 770W (blue), 1000W (green), and 1130W (red) band filters from the JWST (Lee et al. 2022), and overlaid in orange is the continuum subtracted HST-Hα, with CO-rich and CO-poor spur (see Section 3) highlighted in cyan and orange, respectively. Right, top row: from left to right, three-color MIRI (same as left panel) and NIRCam (red: 200W, green: 300M, blue: 335M) zooms of the spurs, as well as MUSE Hα and ALMA CO. Right, middle: from left to right, increasing JWST NIRCam wavelengths, showing the stellar light. Right, bottom: from left to right, increasing JWST MIRI wavelengths, showing the ISM emission.
Paper: PHANGS-JWST First Results: Spurring on Star Formation: JWST Reveals Localized Star Formation in a Spiral Arm Spur of NGC 628
Authors: Thomas G. Williams, Jiayi Sun, Ashley T. Barnes, Eva Schinnerer, Jonathan D. Henshaw, Sharon E. Meidt, Miguel Querejeta, Elizabeth J. Watkins, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Mélanie Chevance, Oleg V. Egorov, Eric Emsellem, Simon C. O. Glover, Kathryn Grasha, Hamid Hassani, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Ismael Pessa, Jérôme Pety, Francesca Pinna, Erik Rosolowsky, Karin M. Sandstrom, Rowan Smith, Mattia C. Sormani, Sophia Stuber, David A. Thilker, Bradley C. Whitmore
Figure caption: Profiles of 21 μm, Balmer-corrected Hα (equivalent to SFR), CO, and SFE values across the CO-rich and CO-poor spurs (the mask generated from the contours in Figure 1) as a function of galactocentric radius. The solid line shows the rolling median of the data, and the shaded regions the 16th and 84th percentiles. Each intensity is normalized by its 50th percentile value within the spur mask, and is offset for visual clarity. The shaded gray region indicates the parts of the spur within the spiral arm mask. For reference, the offsets are 1, 2, 3, and 4 for 21 μm, SFR, CO, and SFE, respectively. These lines correspond to the median value of 1.6 MJy sr−1 (21 μm), 5.3 × 10−3 M ⊙ kpc−2 (SFR surface density, assuming a Calzetti et al. 2007 conversion factor), 4.7 K km s−1 (CO), and 3.4 × 10−7 yr−1 (SFE) for the CO-rich spur, and 1.2 MJy sr−1, 4.2 × 10−3 M ⊙ kpc−2, 3.7 K kms−1, and 3.3× 10−7 yr−1 for the CO-poor spur.
Paper: PHANGS-JWST First Results: Spurring on Star Formation: JWST Reveals Localized Star Formation in a Spiral Arm Spur of NGC 628
Authors: Thomas G. Williams, Jiayi Sun, Ashley T. Barnes, Eva Schinnerer, Jonathan D. Henshaw, Sharon E. Meidt, Miguel Querejeta, Elizabeth J. Watkins, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Mélanie Chevance, Oleg V. Egorov, Eric Emsellem, Simon C. O. Glover, Kathryn Grasha, Hamid Hassani, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Ismael Pessa, Jérôme Pety, Francesca Pinna, Erik Rosolowsky, Karin M. Sandstrom, Rowan Smith, Mattia C. Sormani, Sophia Stuber, David A. Thilker, Bradley C. Whitmore
Figure caption: Polar deprojection of NGC 628 in CO (top), 21 μm (middle), and MUSE Hα (bottom). 0° is defined as the position angle (see Figure 1), and θ increases from left to right. The nominal corotation radius from Williams et al. (2021) is shown as a horizontal dashed white line. We show the approximate ridge of three spiral arms as red lines (determined from the CO). We note there is a clear offset between this CO ridge and the 21 μm/Hα ridges (see also, e.g., Kreckel et al. 2018) The cyan contour indicates the “CO-rich” spur, and the orange the “CO-poor” spur.
Paper: PHANGS-JWST First Results: Spurring on Star Formation: JWST Reveals Localized Star Formation in a Spiral Arm Spur of NGC 628
Authors: Thomas G. Williams, Jiayi Sun, Ashley T. Barnes, Eva Schinnerer, Jonathan D. Henshaw, Sharon E. Meidt, Miguel Querejeta, Elizabeth J. Watkins, Frank Bigiel, Guillermo A. Blanc, Médéric Boquien, Yixian Cao, Mélanie Chevance, Oleg V. Egorov, Eric Emsellem, Simon C. O. Glover, Kathryn Grasha, Hamid Hassani, Sarah Jeffreson, María J. Jiménez-Donaire, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Adam K. Leroy, Daizhong Liu, Ismael Pessa, Jérôme Pety, Francesca Pinna, Erik Rosolowsky, Karin M. Sandstrom, Rowan Smith, Mattia C. Sormani, Sophia Stuber, David A. Thilker, Bradley C. Whitmore
Figure caption: Offset timescale (see Equation (1)) as a function of galactocentric radius for the CO-rich (blue) and CO-poor (red) spurs, calculated between a galactocentric radius of 3 and 4 kpc.