Latest Images

A spectrum from a spaxel near the optocenter is...

A spectrum from a spaxel near the optocenter is shown. The complete spectrum is displaye...

Anita L. Cochran et al, The Planetary Science Journal 7 9

The column densities for CN are shown as a func...

The column densities for CN are shown as a function of distance to the optocenter. We co...

Anita L. Cochran et al, The Planetary Science Journal 7 9

The spatial distribution of the CN fluxes on th...

The spatial distribution of the CN fluxes on the IFU FOV is shown. The position of the o...

Anita L. Cochran et al, The Planetary Science Journal 7 9

The column densities for CN, C3, CH, and C2 (tw...

The column densities for CN, C3, CH, and C2 (two bands) are shown as a function of dista...

Anita L. Cochran et al, The Planetary Science Journal 7 9

The column densities of three of the Ni I lines...

The column densities of three of the Ni I lines are shown as a function of cometocentric...

Anita L. Cochran et al, The Planetary Science Journal 7 9

The column densities of four groups of Fe I lin...

The column densities of four groups of Fe I lines are shown as a function of cometocentr...

Anita L. Cochran et al, The Planetary Science Journal 7 9

Final frames of avalanching simulations for all...

Final frames of avalanching simulations for all of the material compositions, magnetic f...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

Comparison of magnetic force for different fiel...

Comparison of magnetic force for different field strengths (B = 0.5, 50 and 200 μT) with...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

Simulation setup: the frozen floor particles in...

Simulation setup: the frozen floor particles in a hexagonal packing are shown in green, ...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

Final frame of avalanching of non-susceptible w...

Final frame of avalanching of non-susceptible with no magnetic field. Red particles are ...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

Trends of mean angle of repose (...

Trends of mean angle of repose (﹩{\bar{\theta }}_{B}﹩), rms height (﹩\bar{\xi }﹩), and r...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

Perspective views of the final settled avalanch...

Perspective views of the final settled avalanches for 1000 μT field strength in HS-NS 3:...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

Different slices to analyze the angle of repose...

Different slices to analyze the angle of repose, rms height, and rms slope. The simulati...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

Amplification factor vs. magnetic probability P...

Amplification factor vs. magnetic probability P for various susceptibilities χ. The ampl...

Anmol Sikka and Christine M. Hartzell, The Planetary Science Journal 7 9

(Left) View of the final frame of the SCA 5, 3....

(Left) View of the final frame of the SCA 5, 3.4 mag data. The Roman grism disperses lig...

Lipika Chatur et al, Research Notes of the AAS 10 9

Cutouts of SPHEREx Band 1 images that have brig...

Cutouts of SPHEREx Band 1 images that have bright stars located close to pixel coordinat...

Viraj Karambelkar et al, Research Notes of the AAS 10 9

Radio light curve of SN 2024abup at frequencies...

Radio light curve of SN 2024abup at frequencies shown in Table C1, shown alongside other...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

Comparison of the JWST NIR + MIR spectra of SN ...

Comparison of the JWST NIR + MIR spectra of SN  (+41 days) and SN Ic 2023dbc (+36 days) ...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

JWST spectrum of SN 2024abup at +41 days after ...

JWST spectrum of SN 2024abup at +41 days after V-band maximum, overlaid with r-process e...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

Comparison of the NIR spectrum of SN 2024abup a...

Comparison of the NIR spectrum of SN 2024abup at +41 days with SN 1998bw (F. Patat et al...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

SN 2024abup spectrum (black) along with the mod...

SN 2024abup spectrum (black) along with the model of graphite, silicate, and PAH contrib...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

The SN 2024abup JWST spectrum overlayed with al...

The SN 2024abup JWST spectrum overlayed with all the prominent r-process lines identifie...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

The corner plot for the fit using analytic mode...

The corner plot for the fit using analytic models from W. D. Arnett (1982) and S. Valent...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

SN 2024abup compared to model from SUMO. The mo...

SN 2024abup compared to model from SUMO. The model is able to reproduce several observed...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

SN 2024abup spectrum spanning optical (FLOYDS) ...

SN 2024abup spectrum spanning optical (FLOYDS) to MIR (JWST) +41 days after the V-band m...

Manisha Shrestha et al, The Astrophysical Journal Letters 1009 2

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Updated Search and Sort

We have updated the search and sort algorithm to return records in reverse chronological order based on the date/time that the images were uploaded to the Astronomy Image Explorer. This is potentially but rarely different from the publication date. Thank you!