adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: The g-band light curve of AT 2022upj (black line) compared to that of a sample of TDEs (thin gray lines) for which data, with magnitude errors <0.25 mag, exist beyond +200 days from the g-band peak (AT 2018hco, AT 2018iih, AT2018 jbv, AT 2018zr, AT 2019ehz, AT 2020mot, AT 2020opy, AT 2020qhs, AT 2020ysg, AT 2020yue, AT 2021nwa, AT 2022gri, AT 2022lri, and AT 2022wtn; photometry all obtained from J. M. M. Neustadt et al. 2020; S. van Velzen et al. 2021a; E. Hammerstein et al. 2023; J. Li et al. 2023; Y. Yao et al. 2023; J. T. Hinkle et al. 2024; K. I. I. Koljonen et al. 2024). Other ECLEs concurrent with optical transients (AT  2018gn, AT 2018bcb, AT 2018dyk, AT 2021dms, AT 2021acak, and AT 2022fpx) are overplotted in color. AT 2021dms is shown in the ATLAS c band due to the lack of ZTF coverage. All light curves are corrected for each object’s redshift and shown in the rest frame. The TDEs in the background sample show a median power-law decline of α = 2.14 ± 0.96 prior to +200 days from peak (after which a plateau phase is common in TDEs; Y. Yao et al. 2023), while the ECLEs have a power-law decline following α = 0.67 ± 0.22 over the same period, indicating a significant difference between the behavior of long-lasting TDEs vs. ECLEs.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: FLOYDS (unlabeled) and SOAR spectra of AT 2022upj, continuum-normalized and offset with varying hues for clarity. The spectra are labeled by the number of rest-frame days from the optical peak at which the observation was taken. We label the prominent narrow Hα, Hβ, and He II λ4686 lines in gray and the high-ionization coronal lines ([Fe XIV] λ5303, [Fe VII], [Fe x] λ6375, [S XII] λ7611.0, and [Fe XI] λ7891.8) in red. We also label the [O III] λλ4959, 5007 doublet, which is not evident in AT 2022upj until after +190 days from the peak, when [Fe VII] also becomes prominent and the [Fe x] line weakens. These spectra will be available on WISEReP.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Spectral epochs of AT 2022upj from +25 days onward (rest-frame days, since the peak is noted next to each spectrum), each offset and differing in hue for clarity, in which the strong narrow emission lines have been masked, to clearly show the remaining broad feature around He II λ4686, labeled at the line center with a vertical black line and at ±20,000 km s−1 offset with vertical dashed lines. We also show the best-fit Gaussian to each line, with the horizontal dashed line denoting the Gaussian zero level. The red crosses denote the Gaussian centroid for each fit. We find the weighted average of the FWHM across all epochs is 14,700 ± 3400 km s−1.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Unsubtracted WISE photometry at the position of AT 2022upj since 2014. Top: W1 3.6 μm in blue circles and median quiescent value in a darker blue horizontal line. Middle: W2 4.5 μm in pink circles and median quiescent value in a darker pink horizontal line. Bottom: W1 − W2 colors in green pentagons. The host of AT 2022upj never approaches the expected AGN color cut of W1 − W2 > 0.8 until the brightening in both bands after the transient discovery at MJD 59822.39 (marked with the red vertical dashed line).
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Close-up of the first SOAR spectrum of AT 2022upj, focusing on the broad He II λ4686 emission feature, with the same spectral segment shown for the extreme coronal line emitter SDSS 0748+4712 (green; T.-G. Wang et al. 2011) and the TDE AT 2020mot (purple; M. Newsome et al. 2024). SDSS 0748+4712 was the only ECLE from the SDSS sample that simultaneously showed broad He II, making AT 2022upj only the second instance with both features clearly detected and the first for which the detections coincide with an observed optical transient.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Gaussian fits for key emission lines across the four higher-resolution SOAR spectra taken at +25, +30, +406, and +409 rest-frame days from the optical peak. Left: high-ionization lines [O III] λ5007, [Fe XIV] λ5303, [Fe  VIIa], [Fe  VIIb], and [Fe x] λ6375. Right: Hβ, Hα, and the narrow component of He II, for which we treat the broad component as a local continuum. The gray lines are the photometrically calibrated data offset from one another for clarity, and the overlaying purple lines are the Gaussian fits to the data. The first two detections of [O III] and [Fe VII] are less than 3σ detections, as are the last two observations of [Fe XIV].
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: Blackbody physical properties inferred for AT 2022upj (black lines) compared to TDEs (gray lines) and ECLEs (colored lines) for which blackbody data were publicly available (AT2018bcb, AT2018dyk, AT2018hco, AT2018zr, AT2019ehz, and AT2020mot), Top: blackbody luminosity in erg per second. Middle: radius in centimeters. Bottom: temperature in Kelvins. The AT 2022upj luminosity evolution is consistent with TDEs, and its peak radius and temperatures are also in line with TDEs, although there is deviation from both at late times.
Paper: Mapping the Inner 0.1 pc of a Supermassive Black Hole Environment with the Tidal Disruption Event and Extreme Coronal-line Emitter AT 2022upj
Authors: Megan Newsome, Iair Arcavi, D. Andrew Howell, Curtis McCully, Giacomo Terreran, Griffin Hosseinzadeh, K. Azalee Bostroem, Yael Dgany, Joseph Farah, Sara Faris, Estefania Padilla-Gonzalez, Craig Pellegrino, Moira Andrews
Figure caption: X-ray flux (red diamonds) from Swift XRT alongside the photometrically calibrated fluxes of the prominent emission lines [Fe x] λ6375 (dark orange small dots), [Fe XIV] λ5303 λ5303 (purple stars), [Fe VIIa] (blue diamonds), [Fe VIIb] (green pentagons), and Hα λ6563 (black dots).
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Spatial distribution of the 20 molecular clouds in our sample. The background and associated color bar is the integrated intensity of NH3 (3, 3) from HOPS (A. J. Walsh et al. 2011; C. R. Purcell et al. 2012; S. N. Longmore et al. 2017). The overlays are our 13CO J = 2 → 1 moment 0 maps from ALMA. The clouds G5 at (ℓ, b) = (+5.4, −0.4), Bania 1 (B1; T. M. Bania et al. 1986) at (ℓ, b) = (−5.4, +0.4), and Bania 2 (B2; A. A. Stark & T. M. Bania 1986) at (ℓ, b) = (+3, +0.2) are marked with large orange ellipses. The colored shapes around each of the clouds in our sample correspond to our categories, first mentioned in Section 3 and refined in Section 5.4. The pink diamonds indicate the clouds that are highly turbulent and have no detected star formation; these are the most likely to be in the bar region. The red circles indicate the clouds with detected star formation but low turbulence; these are likely to be typical star-forming regions in the Galactic disk. Lastly, the blue squares indicate the clouds with low turbulence and no detected star formation; these are likely to be typical non-star-forming clouds in the Galactic disk.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: The longitude–velocity (ℓ–v) distribution of the cloud sample overlaid on CO J = 1 → 0 emission from M. Bitran et al. (1997), in blue. The black vertical stripes are the velocity spectra of each of the clouds, located horizontally at the cloud’s longitude. The colored shapes and symbols along each of the velocity spectra are centered on the central velocity of each cloud, and they correspond to the same categories as in Figure 1. The pink diamonds indicate the clouds that are highly turbulent and have no detected star formation; these are the most likely to be in the bar region. The red circles indicate the clouds with detected star formation but low turbulence; these are likely to be typical star-forming regions in the Galactic disk. Lastly, the blue squares indicate the clouds with low turbulence and no detected star formation; these are likely to be typical non-star-forming clouds in the Galactic disk. The approximate locations of several important features are also circled.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Top-down projection view of our cloud distribution. In this cartoon, the bar is at an angle of 30° with respect to the Sun, has a semimajor axis of 3.5 kpc, and a semiminor axis length of 0.75 kpc. The black line along the bar axis extends to a Galactic longitude of ±10° in both directions. The blue curves within the bar and the circle at the center of the bar are cartoon depictions of the bar inflows and the CMZ. The clouds, denoted by the red dots, are placed at their respective distances with uncertainties along the lines of sight, denoted by the light blue dashed lines, as per Table 2. These uncertainties may be underestimates, particularly for kinematic distance measurements, which are highly uncertain at small Galactic longitude; see Section 3 for further discussion. Several clouds, particularly those in the bar, overlap in the diagram and are indistinguishable from other nearby clouds.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Ammonia (3, 3)–(1, 1) rotational temperature (T 13) maps for each cloud, on the same color scale, plotted in Galactic coordinates. Clouds are ordered by Galactic longitude. The light blue boxes indicate the ALMA FOV for the cloud. The pink circles are the 2′ Mopra HOPS beam, each centered on the pixel with peak NH3 (3, 3) integrated intensity. The blue circles in the bottom left corner of each map indicate the 31″ ALMA beam size for comparison. The blue lines in the top right corner of each map indicate a physical size of 1 pc. The uncertainties on these physical sizes may be large as they are proportional to the distance uncertainties.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Formaldehyde temperature maps for each cloud, on the same color scale, plotted in Galactic coordinates. Clouds are ordered by Galactic longitude. The light blue boxes are 1′ boxes centered on the pixel with peak H2CO J = 303 → 202 integrated intensity. The blue circles in the bottom left corner of each map indicate the 31″ beam size. The blue lines in the bottom right corner of each map indicate a physical size of 1 pc. The uncertainties on these physical sizes may be large as they are proportional to the distance uncertainties. Clouds G005.75 and G005.49 do not show any H2CO J = 321 → 220 emission and thus do not have formaldehyde temperature maps.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Derived cloud properties plotted against Galactic longitude. The red diamonds are clouds with 24 μm detections, while the blue circles are clouds without. The ammonia temperatures are the value of the ammonia (3, 3)–(1, 1) temperature maps at the pixel with peak NH3 (3, 3) integrated intensity. The formaldehyde temperatures are the average formaldehyde temperature taken over the 1′ box centered on the pixel with peak H2CO J = 303 → 202 integrated intensity.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Three-color Spitzer images of the clouds with Spitzer detections, with GLIMPSE 4.5 μm, GLIMPSE 8 μm, and MIPSGAL 24 μm in blue, green, and red, respectively, plotted in Galactic coordinates. If the clouds also have H30α detections, the contours show H30α integrated intensity; otherwise, the contours show H2CO J = 303 → 202 integrated intensity. The light blue boxes in each image depict the ALMA FOV. The white lines in the top left corner of each map indicate a physical size of 1 pc. The uncertainties on these physical sizes may be large as they are proportional to the distance uncertainties. The 24 μm data contains artifacts at bright spots, so they are masked by the MIPSGAL processing pipeline.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: H30α integrated intensity maps with white contours, for clouds with detections, calculated as described in Section 2.3. The light blue boxes are 1′ boxes centered on the pixel with peak H30α integrated intensity. The blue circles in the bottom left corner of each map indicate the 31″ beam size. The blue lines in the top left corner of each map indicate a physical size of 1 pc. The uncertainties on these physical sizes may be large as they are proportional to the distance uncertainties. The green arrows indicate the paths along which the PV diagram is calculated.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Correlations between different temperature measures. Mean ﹩{T}_{{{\rm{H}}}_{2}\mathrm{CO}}﹩ denotes the average formaldehyde temperature within a 1′ box centered on the pixel with peak H2CO J = 303 → 202 integrated intensity, whereas Pixel ﹩{T}_{{{\rm{H}}}_{2}\mathrm{CO}}﹩ denotes the formaldehyde temperature at the pixel with maximum NH3 (3, 3) integrated intensity once regridded to the ammonia resolution. T 12 represents the ammonia temperature calculated using NH3 (1, 1) and (2, 2), taken at the pixel with peak NH3 (3, 3) integrated intensity, and T 13 is the ammonia temperature calculated using NH3 (1, 1) and (3, 3) at the same pixel. The dashed blue line in each plot indicates identical temperature estimates.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: H2CO FWHM line width against formaldehyde temperature. Both are calculated over a 1′ box centered on the pixel with peak H2CO J = 303 → 202 emission. The dashed blue line indicates the thermal line width as a function of temperature, Equation (9).
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Same as Figure 12, but with H2CO J = 303 → 202 integrated intensity contours for all clouds.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Comparison of ΣSFR calculated using H30α emission vs. that calculated using 24 μm emission from Spitzer. The blue line assumes the two are equal.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Ammonia emission Boltzmann diagrams for all clouds.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Derived cloud properties plotted against both ammonia and formaldehyde temperatures. The red diamonds are clouds with 24 μm detections, while the blue circles are clouds without. The ammonia temperatures are the value of the ammonia (3, 3)–(1, 1) temperature maps at the pixel with peak NH3 (3, 3) integrated intensity. The formaldehyde temperatures are the average formaldehyde temperature taken over the 1′ box centered on the pixel with peak H2CO J = 303 → 202 integrated intensity.
Paper: Investigating the Potential of LS 5039 as a Triple System Using Fermi-LAT Data
Authors: Lujun Zeng, Mengqing Zhang, Chongyang Ren, Pengfei Zhang, Jingzhi Yan
Figure caption: TS maps in the 0.1–500.0 GeV range, covering a 3° × 3° region centered on 4FGL J1826.2−1450, with γ-ray sources from the 4FGL-DR4 marked by crosses. Left panel: TS map representing γ-ray emissions from 4FGL J1826.2−1450, generated using the best-fit model with the target excluded. Right panel: residual TS map created using the same model, except with 4FGL J1826.2−1450 included.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Top: mass estimate calculated using the integrated intensity of 12CO and an X-factor of 2.3 × 1020 cm−2 (K km s−1)−1 against the mass estimated calculated using the integrated intensity of 13CO using the equation of local thermal equilibrium. The blue circles are the clouds likely to be in the bar region as per the discussion in Section 5.4, and the red diamonds are the clouds likely not in the bar region. The blue line indicates where the two mass estimates are equal. Bottom: ratio of the two mass estimates against Galactic longitude. The colors and symbols are the same as above.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Observed formaldehyde temperature plotted against the estimated temperature from turbulent heating (Equation (25)). The red diamonds are clouds with 24 μm detections, while the blue circles are clouds without. The blue line indicates where the two temperatures are equal. For clouds corresponding to points below the blue line, the turbulence-driven estimated temperature is greater than the observed temperature, so turbulence is (more than) sufficient to explain the observed temperature. For clouds corresponding to points above the blue line, turbulence is insufficient to explain the observed temperature.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Formaldehyde temperature error maps for each cloud, with the same overlays as Figure 8.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Ammonia (3, 3)–(1, 1) temperature error maps for each cloud, with the same overlays as Figure 6.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: Map of the intensity-weighted velocity of H2CO (303–202) for cloud G008.67 (left), the gradient fit to the velocities (right), and the residual velocities after subtracting the gradient (bottom). The gradient likely represents large-scale bulk motions of the cloud, separate from turbulence.
Paper: Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Andy Nilipour, Juergen Ott, David S. Meier, Brian Svoboda, Mattia C. Sormani, Adam Ginsburg, Savannah R. Gramze, Natalie O. Butterfield, Ralf S. Klessen
Figure caption: ΣSFR, as measured by H30α emission, plotted against Mach number. The red points indicate clouds with a significant H30α detection, and the blue points indicate clouds without one, for which an upper limit is given.