adsabs/AstroCLIMB huggingface dataset:
Paper: First Peek with JWST/NIRCam Wide-field Slitless Spectroscopy: Serendipitous Discovery of a Strong [O III]/Hα Emitter at z = 6.11
Authors: Fengwu Sun, Eiichi Egami, Nor Pirzkal, Marcia Rieke, Martha Boyer, Matteo Correnti, Mario Gennaro, Julien Girard, Thomas P. Greene, Doug Kelly, Anton M. Koekemoer, Jarron Leisenring, Karl Misselt, Nikolay Nikolov, Thomas L. Roellig, John Stansberry, Christina C. Williams, Christopher N. A. Willmer
Figure caption: Comparisons of emission-line equivalent widths of NRCJ1631+3008-z6.1 (colored diamonds with black edges) with those of galaxies across z ≃ 0–7. Left: Hβ+[O III] line EW vs. the stellar mass of NRCJ1631+3008-z6.1 compared with those of z ∼ 6.8 galaxies whose EWs are inferred from Spitzer/IRAC [3.6 μm]–[4.5 μm] color (circles; Endsley et al. 2021a, 2021b), and also SDSS-selected galaxies in the local universe (dots; Thomas et al. 2013). Sources at z > 6 are color-coded by their UV-based SFRs. Middle: Hα  EW vs. [O III] λ5007 EW compared with those of extreme emission-line galaxies at z = 1.3–2.4 (squares; Tang et al. 2019). Sources are color-coded by their ionizing photon production efficiency (ξ ion). Right: He II λ4686 EW vs. [O III] λ5007 EW compared with those of extreme emission-line galaxies (hexagons; Senchyna et al. 2017, 2020) and SDSS-selected He II AGNs (dots; Oh et al. 2011; Bär et al. 2017) in the local universe. Sources are color-coded with their Hβ  EWs. Given the low significance of He II λ4686 detection with NRCJ1631+3008-z6.1, we show the 5th, 16th, and 84th percentiles of the likelihood distribution of the He II EW.
Paper: Bridging the Bondi and Event Horizon Scales: 3D GRMHD Simulations Reveal X-shaped Radio Galaxy Morphology
Authors: Aretaios Lalakos, Ore Gottlieb, Nicholas Kaaz, Koushik Chatterjee, Matthew Liska, Ian M. Christie, Alexander Tchekhovskoy, Irina Zhuravleva, Elena Nokhrina
Figure caption: Three-dimensional volume rendering of density at t = 1.2 × 105 R g/c ≃ 0.05 Myr (see Figure 2(d)) illustrates the natural development of X-shaped jet morphology. Gas infall forms an accretion flow (bright red) and launches a pair of relativistic jets (light blue), which propagate vertically and shock the ambient gas (dark red). The older cavities (dark blue), which were inflated by previous misaligned jet activity, buoyantly rise at an angle to the vertically propagating jets, form the X-shaped jet morphology.
Paper: First Peek with JWST/NIRCam Wide-field Slitless Spectroscopy: Serendipitous Discovery of a Strong [O III]/Hα Emitter at z = 6.11
Authors: Fengwu Sun, Eiichi Egami, Nor Pirzkal, Marcia Rieke, Martha Boyer, Matteo Correnti, Mario Gennaro, Julien Girard, Thomas P. Greene, Doug Kelly, Anton M. Koekemoer, Jarron Leisenring, Karl Misselt, Nikolay Nikolov, Thomas L. Roellig, John Stansberry, Christina C. Williams, Christopher N. A. Willmer
Figure caption: Top: JWST/NIRCam short-wavelength (F212N) and long-wavelength (F250M, F322W2, and F444W) cutout images of NRCJ1631-3008-z6.1. Measured source brightness in each filter is shown in the lower-right corner of each plot (in AB mag; 3σ upper limit for nondetection). Bottom: best-fit SED model obtained with CIGALE (black curve; Boquien et al. 2019). Photometric measurements are shown as red circles, and best-fit source brightnesses are shown as open blue squares. The transmission curves of four utilized filters are also plotted for comparison. Note that the transmission of the F322W2 band is computed using the measured grism throughput and is different from that in the JWST User Documentation.
Paper: First Peek with JWST/NIRCam Wide-field Slitless Spectroscopy: Serendipitous Discovery of a Strong [O III]/Hα Emitter at z = 6.11
Authors: Fengwu Sun, Eiichi Egami, Nor Pirzkal, Marcia Rieke, Martha Boyer, Matteo Correnti, Mario Gennaro, Julien Girard, Thomas P. Greene, Doug Kelly, Anton M. Koekemoer, Jarron Leisenring, Karl Misselt, Nikolay Nikolov, Thomas L. Roellig, John Stansberry, Christina C. Williams, Christopher N. A. Willmer
Figure caption: JWST/NIRCam F322W2 direct image and F322W2/F444W 2D spectra of NRCJ1631+3008-z6.1 seen with Grism R (top) and C (bottom). The orientations of direct images have been aligned to the dispersion directions of the two grisms. In the plots of 2D spectra, the expected positions of detectable emission lines are indicated with vertical white lines. [O III] λ λ4959/5007 and Hα  lines can be detected with Grism R and C data separately, confirming the line identification. Two potential clumpy structures (A and B) with a spatial offset of 1.6 ± 0.3 kpc and a velocity offset of 602 ± 105 km s−1 are noted with dashed blue and green circles in direct images, respectively, and the expected locations of corresponding line emissions ([O III], Hα, and [N II]) are shown with dashed circles of the same colors superimposed on the 2D spectra. The PAs of the two clumps with respect to the dispersion directions are also shown in the direct images.
Paper: Evidence that Interaction with the Spacecraft Plasma Wake Generates Plasma Waves Close to the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: David M. Malaspina, Sabrina F. Tigik, Andris Vaivads
Figure caption: Comparison of near-f ce wave power with alignment between the PSP ion wake direction and the solar wind magnetic field direction. (a) Solar wind magnetic field vector components in spacecraft body coordinates. (b) Electric field power spectral density. The lower orange, white, and upper orange lines indicate 0.5 f ce, f ce, and 5 f ce, respectively. (c) The cosine of θ  B,Wake, the angle between the solar wind magnetic field vector and the ion wake direction vector. (d) The integral of the power spectral density in (b) between the frequencies indicated by the two orange lines. (e) Integrated power spectral density as a function of θ  B,Wake. (f) Same as (e), with a narrower range of θ  B,Wake shown.
Paper: Evidence that Interaction with the Spacecraft Plasma Wake Generates Plasma Waves Close to the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: David M. Malaspina, Sabrina F. Tigik, Andris Vaivads
Figure caption: Same format as Figure 1, covering a 24 hr interval on 2022 February 22. For clarity of plotting, red points are not indicated in (d).
Paper: Evidence that Interaction with the Spacecraft Plasma Wake Generates Plasma Waves Close to the Electron Cyclotron Frequency in the Near-Sun Solar Wind
Authors: David M. Malaspina, Sabrina F. Tigik, Andris Vaivads
Figure caption: Same format as Figure 1, covering an 11 hr interval on 2020 June 7.
Paper: The First Detection of a Protostellar CO Outflow in the Small Magellanic Cloud with ALMA
Authors: Kazuki Tokuda, Sarolta Zahorecz, Yuri Kunitoshi, Kosuke Higashino, Kei E. I. Tanaka, Ayu Konishi, Taisei Suzuki, Naoya Kitano, Naoto Harada, Takashi Shimonishi, Naslim Neelamkodan, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: 0.87 mm continuum and CO(3–2) high-velocity emission toward the Spitzer source. (a) Color-scale image shows the 0.87 mm continuum emission. The ellipse at the lower-left corner shows the beam size, 0.″41 × 0.″ 30. Blue and red contours show the CO(3–2) high-velocity wing emission with integrated velocity ranges of 147–158 km s−1 and 168–180 km s−1, respectively (see also dotted lines in panel (b)). The lowest and subsequent contour steps are 6 and 10 K km s−1, respectively. Note that the rms noise level is ∼1.3 K km s−1. (b) The blue and red profiles show the CO blueshifted and redshifted high-velocity emission, respectively, extracted from a 0.″45 radius centered at red/blue crosses in panel (a). The yellow profile shows the SO spectrum at the 0.87 mm continuum peak. Note that the intensity is multiplied by a factor of 5 and then is shifted −5 K for visualization purposes. The black dotted lines indicate the systemic velocity of 163 km s−1 determined by the Gaussian fitting.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Panel 1: Q  ϕ  r 2-scaled H-band observations with a sinh colorbar to emphasize bright emission. Panel 2: inner region of the 12CO non-continuum-subtracted peak intensity map; a sinh colorbar is used to emphasize the bright inner gas spiral. Panel 3: peak velocity map of continuum-subtracted 12CO emission. The magenta dashed circle represents the location of the Doppler flip reported by CP19. Panel 4: our Band 6 continuum observations with a high-pass filter. We masked the bright unresolved inner disk to highlight the emission structure in the ring component; see Appendix A for further details. Overplotted in each panel are the black/white dashed contours from the SPHERE observations at 0.53, 0.61, and 0.69 normalized flux units.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Left: residuals from the known Keplerian velocities, i.e., by subtracting a model where we force the gas velocities to be circular and Keplerian around the center of gravity of the model, assuming a central mass of 2.6 M ⊙ (i.e., the total mass of the binary). Center: best-fit Keplerian rotation subtracted with eddy from moment 1 of our SPH simulation. Right: as in the center panel, but for the continuum-subtracted 12CO observations of HD 100546 presented in this work. The binary induced spiral arms in our SPH simulation produce substantial deviations (∼1 km s−1) from Keplerian rotation over short distances, which appears like a Doppler flip when trying to subtract an estimated velocity field. This is similar to the deviations seen in HD 100546 by CP19.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Large-scale continuum-subtracted CO(2–1) channel maps. We highlight several non-Keplerian features with white arrows and overlay a trace of the southern scattered-light spiral (see Figure 7) with a dashed line. We include a large-scale view of our EDDY model subtraction residuals and highlight with a dashed black contour that a prominent velocity spiral arm in the residual map also coincides with the scattered-light spiral. To ensure these deviations are not background noise, we plot the 5σ value (5 × 1.2 mJy beam−1) with a dashed–dotted gray contour in each channel.
Paper: The First Detection of a Protostellar CO Outflow in the Small Magellanic Cloud with ALMA
Authors: Kazuki Tokuda, Sarolta Zahorecz, Yuri Kunitoshi, Kosuke Higashino, Kei E. I. Tanaka, Ayu Konishi, Taisei Suzuki, Naoya Kitano, Naoto Harada, Takashi Shimonishi, Naslim Neelamkodan, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Upper and lower profiles show the smoothed CO(3–2) spectra at angular resolutions of 1.″7 × 1.″3 and 4.″6 × 4.″3, respectively, in Y246. The extracted position of the profiles is the same as that of the blue cross in Figure 1. The horizontal red lines represent the 3σ rms noise levels of CO(2–1) (upper panel) and CO(3–2) (lower panel) observations toward N83C by Muraoka et al. (2017). The blue vertical lines are the same as those in Figure 1(b).
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Selected non-continuum-subtracted 12CO J = 2–1 channel maps highlighting the deviation from Keplerian velocity at the edge of the disk cavity. The lower limit on the colorbar is set to 15 K. The SPHERE Q  ϕ  image is shown with white dashed contours at 1.3e6, 1.5e6, and 1.7e6 adu. White arrows point to the “kink” as it shifts across each channel map. The magenta dashed circle represents the location of the Doppler flip reported by CP19.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Panel 1: integrated density from our SPH simulation. Panels 2, 3, and 4: synthetic channel maps from our circumbinary model with a ∼0.6 M ⊙ (q = 0.3) companion at 8.4 au convolved with the same beam dimensions as the observations.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Left: Q  ϕ  r 2 H-band observations. Right: peak intensity map of 12CO emission. An asinh scale is applied to both figures to highlight the fainter outer disk emission.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Left: Q  ϕ  r 2-scaled H-band observations. Right: synthetic Q  ϕ  r 2-scaled H-band image produced with MCFOST. For both panels, the flux is normalized to compare the real and synthetic data, and the colorbar is scaled to the power of 4 to solely highlight the bright inner spiral.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Disk surface height for 12CO, extracted using CO LAYERS (Pinte et al. 2018b), where the uncertainty is taken as the vertical deviation in each bin. The scattered-light emission height is taken to be H scat = 0.13 × r 1.08 from Sissa et al. (2018).
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Large-scale continuum-subtracted 13CO and C18O channel maps. We highlight a tentative inner kink in both isotopologues with a white arrow.
Paper: The Origin of the Doppler Flip in HD 100546: A Large-scale Spiral Arm Generated by an Inner Binary Companion
Authors: Brodie J. Norfolk, Christophe Pinte, Josh Calcino, Iain Hammond, Nienke van der Marel, Daniel J. Price, Sarah T. Maddison, Valentin Christiaens, Jean-François Gonzalez, Dori Blakely, Giovanni Rosotti, Christian Ginski
Figure caption: Left: our Band 6 observations. Right: our Band 6 continuum observations with a high-pass filter.
Paper: Two Homologous Quasi-periodic Fast-mode Propagating Wave Trains Induced by Two Small-scale Filament Eruptions
Authors: Jincheng Wang, Xiaoli Yan, Zhike Xue, Liheng Yang, Qiaoling Li, Zhe Xu, Liping Yang, Yang Peng
Figure caption: Time–distance diagrams constructed by SDO/AIA 193 Å running-difference maps. (a) Time–distance diagram along sector S1 in Figure 1(b2) for the first event. (b) The zoom-in region marked by the yellow box in panel (a). (c) Time–distance diagram along sector S2 in Figure 2(b2) for the second event. (d) The zoom-in region marked by the yellow box in panel (c). The white lines in panels (b) and (c) denote the signals of QFP wave trains.
Paper: Two Homologous Quasi-periodic Fast-mode Propagating Wave Trains Induced by Two Small-scale Filament Eruptions
Authors: Jincheng Wang, Xiaoli Yan, Zhike Xue, Liheng Yang, Qiaoling Li, Zhe Xu, Liping Yang, Yang Peng
Figure caption: Wavelet analysis of the detrended flux of 94 and 335 Å intensity peak in the flare kernel. (a1, b1) Wavelet powers derived from the detrended flux of 94 and 335 Å intensity peaks for the first QFP wave train. (a2, b2) Wavelet powers derived from the detrended flux of 94 and 335 Å intensity peaks for the second QFP wave train. The dotted–dashed line in global power indicates the 95% significance level. (c1, c2) SDO/AIA 335 Å maps at 07:27:36 UT and 19:14:36 UT. The pixels of intensity peaks are depicted by black colors, marked by the red arrow. Yellow and blue contours are line-of-sight magnetic fields with levels of ±100 G, respectively.
Paper: Two Homologous Quasi-periodic Fast-mode Propagating Wave Trains Induced by Two Small-scale Filament Eruptions
Authors: Jincheng Wang, Xiaoli Yan, Zhike Xue, Liheng Yang, Qiaoling Li, Zhe Xu, Liping Yang, Yang Peng
Figure caption: Variations of 94 and 335 Å intensity peaks in the flare kernel. (a1, a2) Profiles of intensity peaks in 94 and 335 Å passbands. The upper part is superimposed by the time–distance diagrams of the 193 Å running-difference map. The red lines are the smoothed intensity peaks using a 60 s boxcar. (b1, b2) Variations of detrended flux of 94 Å intensity peak. (c1, c2) Variations of detrended flux of 335 Å intensity peak. The detrended flux is derived by subtracting the smoothed data (see the red lines in panels (a1) and (b1)) from the original intensity. Panels (a1), (b1), and (c1) are for the first QFP wave train, while panels (a2), (b2), and (c2) are for the second QFP wave train.
Paper: Bridging the Bondi and Event Horizon Scales: 3D GRMHD Simulations Reveal X-shaped Radio Galaxy Morphology
Authors: Aretaios Lalakos, Ore Gottlieb, Nicholas Kaaz, Koushik Chatterjee, Matthew Liska, Ian M. Christie, Alexander Tchekhovskoy, Irina Zhuravleva, Elena Nokhrina
Figure caption: Northern jet transitions from cylindrical shape at early times to parabolic shape at late times (southern jet shows qualitatively similar behavior; not shown). Lines of different colors and thicknesses indicate different times (see legend). At early times, t ≲ 0.03 Myr, the jets exhibit a cylindrical shape at z ≳ 10R g: the ram pressure is high (large ﹩\dot{M}﹩ in Figure 1(a)) and BH magnetic flux and jet power are low (small ϕ BH and η in Figures 1(b) and (d)), leading to strong collimation of the jets. At later times, after enough magnetic flux has accumulated on the BH, the jets become stronger and take on a parabolic shape. We compute the cylindrical radius of the jet via the solid angle subtended by the jet (which we identify here as the region of μ > 1.5).
Paper: Bridging the Bondi and Event Horizon Scales: 3D GRMHD Simulations Reveal X-shaped Radio Galaxy Morphology
Authors: Aretaios Lalakos, Ore Gottlieb, Nicholas Kaaz, Koushik Chatterjee, Matthew Liska, Ian M. Christie, Alexander Tchekhovskoy, Irina Zhuravleva, Elena Nokhrina
Figure caption: Synthetic bolometric X-ray images (emissivity P  X  ∝ ρ 2 T 1/2, ignoring absorption and scattering) demonstrate the formation of X-shaped jet morphology. Shock compressed and heated regions dominate the Bremsstrahlung emission, whereas empty cavities show jets or jet-inflated cavities. These low-emission regions present a morphology similar to X-shaped jets in XRGs. The color depicts the emissivity normalized by its angle-averaged value (Section 3.3). Each row and column corresponds to a different inclination angle and time, respectively. Times and lengths shown in each panel have been scaled to M87* (see also Figure 2).
Paper: Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
Authors: Sara Tomita, Yutaka Ohira, Shigeo S. Kimura, Kengo Tomida, Kenji Toma
Figure caption: Density distribution, n/n 0, in the shock downstream region at t = 2t esc for n cl/n 0 = 2 (top two panels) and n cl/n 0 = 20 (bottom two panels). The time, t, represents the elapsed time since the clump has interacted with the shock front. The left and right columns show the results for the PIC and MHD simulations, respectively. Movie: https://docs.google.com/presentation/d/1cseAc5ehoR-9V917zVC_lzvVw9Pi3a8Q/edit?usp=sharing&ouid=112346314884784410578&rtpof=true&sd=true.
Paper: Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
Authors: Sara Tomita, Yutaka Ohira, Shigeo S. Kimura, Kengo Tomida, Kenji Toma
Figure caption: The same as Figure 2, but for the magnetic field strength (B − 4B 0)/4B 0 (left column) and the ratio of B  x  to B  y , ∣B  x /B  y ∣ − 1 (right column).
Paper: Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
Authors: Sara Tomita, Yutaka Ohira, Shigeo S. Kimura, Kengo Tomida, Kenji Toma
Figure caption: The time evolution of the maximum magnetic field amplification factor in the shock downstream region, ﹩({B}_{\max }-4{B}_{0})/4{B}_{0}﹩. The time, t, represents the elapsed time since the clump has interacted with the shock front. The open and filled points show the results for n cl/n 0 = 2 and 20, respectively. The squares and circles show the results for the MHD and PIC simulations, respectively.
Paper: Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
Authors: Sara Tomita, Yutaka Ohira, Shigeo S. Kimura, Kengo Tomida, Kenji Toma
Figure caption: The x component of four velocity at the high-density clump, u  x , at t = 2t esc, as a function of the density of the clump, n cl/n 0. The triangles, squares, and circles show the results for the GSD approximation, the MHD simulation, and the PIC simulation, respectively.
Paper: Interaction of a Relativistic Magnetized Collisionless Shock with a Dense Clump
Authors: Sara Tomita, Yutaka Ohira, Shigeo S. Kimura, Kengo Tomida, Kenji Toma
Figure caption: The same as Figure 2, but for the z component of vorticity, ﹩{(\vec{{\rm{\nabla }}}\times {\boldsymbol{u}})}_{z}﹩.
Paper: The JWST Early Release Observations
Authors: Klaus M. Pontoppidan, Jaclyn Barrientes, Claire Blome, Hannah Braun, Matthew Brown, Margaret Carruthers, Dan Coe, Joseph DePasquale, Néstor Espinoza, Macarena Garcia Marin, Karl D. Gordon, Alaina Henry, Leah Hustak, Andi James, Ann Jenkins, Anton M. Koekemoer, Stephanie LaMassa, David Law, Alexandra Lockwood, Amaya Moro-Martin, Susan E. Mullally, Alyssa Pagan, Dani Player, Charles Proffitt, Christine Pulliam, Leah Ramsay, Swara Ravindranath, Neill Reid, Massimo Robberto, Elena Sabbi, Leonardo Ubeda, Michael Balogh, Kathryn Flanagan, Jonathan Gardner, Hashima Hasan, Bonnie Meinke, Antonella Nota
Figure caption: MIRI MRS spectrum of the central 0.65″ radius region surrounding the central Seyfert nucleus of NGC 7319. A selection of key atomic and molecular emission features have been labeled.