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Paper: Detection of Hidden Emissions in Two Rotating Radio Transients with High Surface Magnetic Fields
Authors: S. B. Zhang, X. Yang, J. J. Geng, Y. P. Yang, X. F. Wu
Figure caption: Pulse trains of J1854+0306 (left) and J1846-0257 (right): for each panel, left is the train of individual pulses for all periods, with the peak flux of each single pulse plotted immediately to the right; the top-right shows the train of pulses for periods with a peak flux-to-noise ratio <5; the bottom-right is the train of pulses for periods with a peak flux-to-noise ratio <3. The stacks of the weak emissions for J1854+0306 and J1846-0257 are folded over 50 and 100 rotation periods, respectively. The Y-axis labeled “Period Index” corresponds to the folded time index based on pulsar periods. Each subplot also presents the mean profile at the top.
Paper: Detection of Hidden Emissions in Two Rotating Radio Transients with High Surface Magnetic Fields
Authors: S. B. Zhang, X. Yang, J. J. Geng, Y. P. Yang, X. F. Wu
Figure caption: Pulse trains of J1839-0141 (left) and J1913+1330 (right): for each panel, the top displays the train of individual pulses for all periods, with the peak flux of each single pulse plotted immediately to the right; the bottom is the train of pulses for periods with peak flux-to-noise ratio <5. The stacks of the weak emissions for J1839-0141 and J1913+1330 have been folded over 100 rotation periods. The Y-axis labeled “Period Index” corresponds to the folded time index based on pulsar periods. Each subplot also presents the mean profile at the top.
Paper: Detection of Hidden Emissions in Two Rotating Radio Transients with High Surface Magnetic Fields
Authors: S. B. Zhang, X. Yang, J. J. Geng, Y. P. Yang, X. F. Wu
Figure caption: Period vs. period derivative for pulsars with radio emission, RRATs, pulsars with giant pulses, and the RRATs observed in this study. RRATs with relatively high Bs studied in our study (J1846-0257 and J1854+0306) are represented by red-filled stars, while RRATs with regular Bs (J1839-0141 and J1913+1330) are denoted by black-filled stars. Pulsars with giant pulses (J0534+2200; M. V. Popov et al. 2006; J0540-6919; M. Geyer et al. 2021) are indicated by green-filled circles. Gray dashed lines represent constant surface magnetic flux density, while gray dotted lines represent constant spin-down age. The inset gives a closer look at the sources around the RRATs with relatively high Bs (J1846-0257 and J1854+0306).
Paper: Detection of Hidden Emissions in Two Rotating Radio Transients with High Surface Magnetic Fields
Authors: S. B. Zhang, X. Yang, J. J. Geng, Y. P. Yang, X. F. Wu
Figure caption: Polarization properties of J1854+0306. The upper panel displays the position angle of linear polarization at 1250 MHz, with red circles and blue stars representing strong RRAT emission and sequential weak emission, respectively. The component numbers are indicated. The lower panel presents the integrated polarization pulse profile, where the red and blue curves correspond to strong RRAT emission and sequential weak emission. Solid lines represent total intensity, while dashed lines indicate linear polarization. The inset provides a detailed view of the polarization profile of the sequential weak emission.
Paper: Detection of Hidden Emissions in Two Rotating Radio Transients with High Surface Magnetic Fields
Authors: S. B. Zhang, X. Yang, J. J. Geng, Y. P. Yang, X. F. Wu
Figure caption: Normalized fluence distributions of single pulses from RRAT J1913+1330, J1846-0257, and J1854+0306, as well as giant pulses from the Crab pulsar and J0540-6919. The fluence values for each source are normalized to their brightest bursts. Density represents the number of bursts per bin divided by the total detected bursts.
Paper: Detection of Hidden Emissions in Two Rotating Radio Transients with High Surface Magnetic Fields
Authors: S. B. Zhang, X. Yang, J. J. Geng, Y. P. Yang, X. F. Wu
Figure caption: Polarization properties of strong RRAT emissions of J1854+0306 and J1846-0257: in each subplot, the upper panel displays the position angle of linear polarization at 1250 MHz. The component numbers are indicated. The middle panel presents the polarization pulse profile, with the red solid line, red dashed line, and blue dashed line denoting total intensity, linear polarization, and circular polarization. The lower panel is the phase-normalized flux density for individual strong RRAT pulses.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: 68% and 95% marginalized contours in the w 0,DE–∑m  ν  [eV] (top) and w  a,DE–∑m  ν  [eV] (bottom) planes for different data combinations.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: Comparison of 1D marginalized posterior distributions for ∑m  ν  [eV] for different data combinations. The two vertical gray dashed lines correspond to 0.057 eV and 0.096 eV, which are the minimum masses required by normal and inverted hierarchies, respectively.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: 68% and 95% marginalized contours in the H 0–N eff (top) and H 0–∑m  ν  [eV] (bottom) planes for different data combinations.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: 68% and 95% marginalized contours in the w 0,DE–w  a,DE plane for different data combinations. The region at the bottom of the vertical dashed black line and above the slanted dashed black line is the parameter space for quintessence-like/non-phantom DE.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: The top panel shows the 1D marginalized posterior probability distributions for A lens for different data combinations. The bottom panel shows the 68% and 95% marginalized contours in the A lens–∑m  ν  [eV] plane for the same data combinations.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: Comparison of 1D marginalized posterior probability distributions for the the Hubble constant H 0 (km s−1 Mpc−1) for different data combinations.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: Comparison of 1D marginalized posterior probability distributions for w 0 and w  a  for different data combinations.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: The top panel shows the 1D marginalized posterior probability distributions for N eff for different data combinations. The bottom panel shows the 68% and 95% marginalized contours in the N eff–∑m  ν  [eV] plane for the same data combinations. The vertical dashed line in the top panel corresponds to ﹩{N}_{\mathrm{eff}}^{\mathrm{SM}}=3.044﹩.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: Comparison of 1D marginalized posterior probability distributions for the running of the scalar spectral index α  s  for different data combinations.
Paper: Updated Cosmological Constraints in Extended Parameter Space with Planck PR4, DESI Baryon Acoustic Oscillations, and Supernovae: Dynamical Dark Energy, Neutrino Masses, Lensing Anomaly, and the Hubble Tension
Authors: Shouvik Roy Choudhury, Teppei Okumura
Figure caption: 68% and 95% marginalized contours in the ﹩{{\rm{\Omega }}}_{m}\unicode{8210}\sqrt{0.3}{S}_{8}﹩ plane, where ﹩{S}_{8}\equiv {\sigma }_{8}{({{\rm{\Omega }}}_{m}/0.3)}^{0.5}﹩, for different data combinations.
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: Color-excess ratios β  λ  = E(K − λ)/E(H − K) as a function of wavelength for the four dense cloud cores L429, L483, L673, and L1165 are shown with various colored markers. The extinction laws predicted by WD01 for R  V  = 3.1 and R  V  = 5.5 are represented by dashed and dotted lines, respectively, while the Astrodust model by HD23 is depicted with a solid line. For comparison, the observed extinction law for the diffuse ISM toward Cyg OB2-12 is shown with a dotted–dashed line from B. S. Hensley & B. T. Draine (2020; hereafter HD20). The measurements from J. Ascenso et al. (2013) for the dense cores B59 and FeSt1-457 are shown in gray markers. The inset is a zoomed-in view of the MIR regime.
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: The extinction law A  λ /A  K  for the four dense cloud cores L429, L483, L673, and L1165 (colored circles) alongside results from WD01 for R  V  = 3.1 (dashed line) and R  V  = 5.5 (dotted line), HD20 for Cyg OB2-12 (dashed–dotted line), and HD23 for Astrodust (solid line). Some other observational results are shown as colored markers for comparison (R. Indebetouw et al. 2005, S. Wang & X. Chen 2019; J. L. Sanders et al. 2022; J. Li et al. 2024a).
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: (a) The extinction law A  λ /A  K  calculated from spherical grains with radii a = 0.01 (solid lines), 0.1 (dashed lines), and 0.3 μm (dotted lines) of silicate (black) and graphite (gray) composition. The optical constants of silicate and graphite are taken from B. T. Draine & H. M. Lee (1984). (b) The extinction law A  λ /A  K  calculated from a mixture of silicate and graphite with a power-law size distribution ﹩{dn}/{da}\propto {a}^{-3.5}﹩ (J. S. Mathis et al. 1977), with ﹩{a}_{\min }=0.005\,\mu {\rm{m}}﹩ and ﹩{a}_{\max }﹩=0.25 μm (black solid line), 0.5 (gray dashed line), 1.0 (orange dotted–dashed line), 2.5 (magenta dotted line), and 10 μm (purple solid line). The colored circles present the observed extinction A  λ /A  K  of the four dense cores L429, L483, L673, and L1165.
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: UKIDSS color–color diagrams (J − H) vs. (H − K) for the four dense cloud cores L429, L483, L673, and L1165. The red solid lines represent the best-fit linear relations obtained using the LTS_LINEFIT method, while the green dashed and dotted lines indicate the 1σ and 3σ confidence intervals of the fits, respectively. The gray markers denote outliers identified by the LTS_LINEFIT algorithm. Best-fit parameters, including the slope and intercept, are displayed in the upper-left corner of each panel.
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: Color–color diagrams of (K − λ) vs. (H − K) for UKIDSS and Spitzer/IRAC for L673, where λ corresponds to IRAC [3.6] (top left), [4.5] (top right), [5.8] (lower left), and [8.0] (lower right). The red solid lines represent the best-fit linear relations for each band, as determined by the LTS_LINEFIT method.
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: Analogous to Figure 2 but for the L429 core.
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: Analogous to Figure B1 but for the L483 core.
Paper: Discovery of a Rare Group of Dwarf Galaxies in the Local Universe
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Pierre-Alain Duc, Jaewon Yoo, Oliver Müller
Figure caption: The BTFR plotted as total baryonic mass against σ 3D of dwarf galaxy groups. For comparison, we plot the total baryonic mass against the rotation velocity of galaxies from L16. The S17 sample is shown by red circles, where the blue dots represent the triplet group. The best-fit value of L16 data shown by a solid line and the dashed line is derived from the cosmic baryon fraction using the equation ﹩{M}_{200}{f}_{b}\propto {M}_{200}^{3}{f}_{V}^{3}﹩, with a value of f  b  = 0.17 and f  V  = 1. Our group (green circles) stands out, being a significant outlier on the left side of the BTFR, and nearly falls along the line of the cosmic average baryon fraction.
Paper: Discovery of a Rare Group of Dwarf Galaxies in the Local Universe
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Pierre-Alain Duc, Jaewon Yoo, Oliver Müller
Figure caption: The position of the member galaxies (black asterisk) in a phase-space diagram. For comparison, we use the S17 groups, where different colors represent different groups, and their respective group dynamical masses (Log(M dyn/M ☉)) are listed in the legend. The solid, dashed, and dashed–dotted lines represent the escape velocity curve for a halo mass of 1010, 1011, and 1011.5 M ☉, respectively.
Paper: Discovery of a Rare Group of Dwarf Galaxies in the Local Universe
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Pierre-Alain Duc, Jaewon Yoo, Oliver Müller
Figure caption: The g − r − z combined color image cutout of the system obtained from the Legacy survey viewer page. The five member dwarf galaxies are designated, and we also provide their redshift information. All five members are arranged in almost a vertical straight line spanning from north to south. The most massive galaxy is a face-on spiral galaxy, D2, which has a B-band absolute luminosity of −16.71 mag.
Paper: Discovery of a Rare Group of Dwarf Galaxies in the Local Universe
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Pierre-Alain Duc, Jaewon Yoo, Oliver Müller
Figure caption: A zoomed-in view of the member galaxies. The 1′ × 1′ square box is zoomed in to a better view, where we marked the central positions with the black dots. The red and blue dots represent the redshifted and blueshifted parts of the galaxy with respect to their center, respectively.
Paper: Discovery of a Rare Group of Dwarf Galaxies in the Local Universe
Authors: Sanjaya Paudel, Cristiano G. Sabiu, Suk-Jin Yoon, Pierre-Alain Duc, Jaewon Yoo, Oliver Müller
Figure caption: The DESI EDR optical spectra of the central region of member galaxies. The observed spectra are shifted to the rest-frame wavelength and smoothed with a three-pixel Gaussian kernel. The major emission lines are marked with vertical dash lines.
Paper: The Flattest Infrared Extinction Curve in Four Isolated Dense Molecular Cloud Cores
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, He Zhao, 赫 赵, Botao Jiang, 博韬 江, Xi Chen, 曦 陈
Figure caption: Analogous to Figure B1 but for the L1165 core.
Paper: Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4
Authors: Erica Nelson, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, Alice E. Shapley, Katherine E. Whitaker, Emily Wisnioski, Natascha M. Förster Schreiber, Renske Smit, Pieter van Dokkum, John Chisholm, Ryan Endsley, Abigail I. Hartley, Justus Gibson, Emma Giovinazzo, Garth Illingworth, Ivo Labbe, Michael V. Maseda, Jorryt Matthee, Alba Covelo Paz, Sedona H. Price, Naveen A. Reddy, Irene Shivaei, Andrea Weibel, Stijn Wuyts, Mengyuan Xiao, Stacey Alberts, William M. Baker, Andrew J. Bunker, Alex J. Cameron, Stephane Charlot, Daniel J. Eisenstein, Anna de Graaff, Zhiyuan Ji, Benjamin D. Johnson, Gareth C. Jones, Roberto Maiolino, Brant Robertson, Lester Sandles, Katherine A. Suess, Sandro Tacchella, Christina C. Williams, Joris Witstok
Figure caption: Velocity gradient. As described in Section 3, we fit the light-weighted center along the x-axis in the grism image, which corresponds to the dispersion direction (top left) and medium band Hα image (top right). The grism has a spectral resolution of R ∼ 1600, meaning that the grism spectrum contains both spatial and spectral information across the dispersion direction. The difference between the grism and direct image centroids is the velocity in that spatial pixel. The error bars on the velocity curve are given by the difference between using the rest-UV emission and the F444W direct image.
Paper: Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4
Authors: Erica Nelson, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, Alice E. Shapley, Katherine E. Whitaker, Emily Wisnioski, Natascha M. Förster Schreiber, Renske Smit, Pieter van Dokkum, John Chisholm, Ryan Endsley, Abigail I. Hartley, Justus Gibson, Emma Giovinazzo, Garth Illingworth, Ivo Labbe, Michael V. Maseda, Jorryt Matthee, Alba Covelo Paz, Sedona H. Price, Naveen A. Reddy, Irene Shivaei, Andrea Weibel, Stijn Wuyts, Mengyuan Xiao, Stacey Alberts, William M. Baker, Andrew J. Bunker, Alex J. Cameron, Stephane Charlot, Daniel J. Eisenstein, Anna de Graaff, Zhiyuan Ji, Benjamin D. Johnson, Gareth C. Jones, Roberto Maiolino, Brant Robertson, Lester Sandles, Katherine A. Suess, Sandro Tacchella, Christina C. Williams, Joris Witstok
Figure caption: Star-forming main sequence for galaxies with grism spectroscopic redshifts 4.5 < z < 6 in FRESCO with detected Hα. SFRs are computed from the measured Hα fluxes corrected for dust attenuation using empirical relations based on the UV slope (I. Shivaei et al. 2020). A fit to the SFMS from J. S. Speagle et al. (2014) is indicated by the red line for context. The typical measurement error is indicated by the plus sign in the lower right corner. Twister-z5, the galaxy featured in the present study, is at the very massive end of this distribution on the upper end of a continuation of the locus of points.
Paper: Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4
Authors: Erica Nelson, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, Alice E. Shapley, Katherine E. Whitaker, Emily Wisnioski, Natascha M. Förster Schreiber, Renske Smit, Pieter van Dokkum, John Chisholm, Ryan Endsley, Abigail I. Hartley, Justus Gibson, Emma Giovinazzo, Garth Illingworth, Ivo Labbe, Michael V. Maseda, Jorryt Matthee, Alba Covelo Paz, Sedona H. Price, Naveen A. Reddy, Irene Shivaei, Andrea Weibel, Stijn Wuyts, Mengyuan Xiao, Stacey Alberts, William M. Baker, Andrew J. Bunker, Alex J. Cameron, Stephane Charlot, Daniel J. Eisenstein, Anna de Graaff, Zhiyuan Ji, Benjamin D. Johnson, Gareth C. Jones, Roberto Maiolino, Brant Robertson, Lester Sandles, Katherine A. Suess, Sandro Tacchella, Christina C. Williams, Joris Witstok
Figure caption: Top left: 1D spectrum of Twister-z5. Top right: three-color image F444W/F200W/F090W. Bottom left: photometry and best-fit stellar population synthesis model for Twister-z5. Bottom right: photometric redshift probability distribution function.
Paper: Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4
Authors: Erica Nelson, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, Alice E. Shapley, Katherine E. Whitaker, Emily Wisnioski, Natascha M. Förster Schreiber, Renske Smit, Pieter van Dokkum, John Chisholm, Ryan Endsley, Abigail I. Hartley, Justus Gibson, Emma Giovinazzo, Garth Illingworth, Ivo Labbe, Michael V. Maseda, Jorryt Matthee, Alba Covelo Paz, Sedona H. Price, Naveen A. Reddy, Irene Shivaei, Andrea Weibel, Stijn Wuyts, Mengyuan Xiao, Stacey Alberts, William M. Baker, Andrew J. Bunker, Alex J. Cameron, Stephane Charlot, Daniel J. Eisenstein, Anna de Graaff, Zhiyuan Ji, Benjamin D. Johnson, Gareth C. Jones, Roberto Maiolino, Brant Robertson, Lester Sandles, Katherine A. Suess, Sandro Tacchella, Christina C. Williams, Joris Witstok
Figure caption: We infer the spatial distribution of Hα (right) from the difference between the F444W broadband filter (center) and F410M medium-band filter (left), which covers the Hα emission line at this redshift. The circle in the middle panel shows the size (FWHM) of the PSF.
Paper: Ionized Gas Kinematics with FRESCO: An Extended, Massive, Rapidly Rotating Galaxy at z = 5.4
Authors: Erica Nelson, Gabriel Brammer, Clara Giménez-Arteaga, Pascal A. Oesch, Rohan P. Naidu, Hannah Übler, Jasleen Matharu, Alice E. Shapley, Katherine E. Whitaker, Emily Wisnioski, Natascha M. Förster Schreiber, Renske Smit, Pieter van Dokkum, John Chisholm, Ryan Endsley, Abigail I. Hartley, Justus Gibson, Emma Giovinazzo, Garth Illingworth, Ivo Labbe, Michael V. Maseda, Jorryt Matthee, Alba Covelo Paz, Sedona H. Price, Naveen A. Reddy, Irene Shivaei, Andrea Weibel, Stijn Wuyts, Mengyuan Xiao, Stacey Alberts, William M. Baker, Andrew J. Bunker, Alex J. Cameron, Stephane Charlot, Daniel J. Eisenstein, Anna de Graaff, Zhiyuan Ji, Benjamin D. Johnson, Gareth C. Jones, Roberto Maiolino, Brant Robertson, Lester Sandles, Katherine A. Suess, Sandro Tacchella, Christina C. Williams, Joris Witstok
Figure caption: Velocity dispersion profile. As described in Section 3, the width of the Hα line in the spectral direction is broadened by three things: the line-of-sight velocity dispersion of the Hα gas (including beam smearing), the spectrograph line-spread function, and the intrinsic spatial extent. To measure the line-of-sight velocity dispersion, we subtract the latter two terms off in quadrature. Twister-z5 has a centrally peaked velocity dispersion cospatial with centrally concentrated light, perhaps indicative of a bulge. We measure a disk velocity dispersion of 50–150 km s−1, which is likely an upper limit because dynamical forward-modeling has not been performed. The fact that the velocity dispersion peaks in the center and is lower in the disk suggests that the observed velocity gradient is likely due to rotation as opposed to a merger (for which one would expect peaks in the velocity dispersion on either side).