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Table of Contents

• Basic information
• Infrared Fluxes
• Spectral Energy Distributions
• Infrared Images
• Infrared Spectra
• Spitzer Observations
• Further Reading

Basic Information

• Common name: M57

• Other names: NGC 6720, IRAS 18517+3257

• Position: RA= 18h53m35.16s Dec=+33d02m43.2s (J2000)

• Type: planetary nebula

• Distance: d= 400 parsecs (Sabbadin, 1986A&AS, 160, 31)

As the prototypical planetary nebula, M57 has been extensively studied through all wavelengths by astronomers. ISO 15 micron imaging of M57 was obtained to study the distribution of cold dust within the nebula. The cold dust allows observers to map the mass loss history of the progenitor star on a larger time scale than that derived from optical observations. Physical processes such as shocks within the nebula caused by winds are evident from spectral fine structure lines detected with ISO LWS.

Infrared Fluxes

Spectral Energy Distributions

This SED was created using the sensitivity and saturation values available in November 2004. The black dots are the object surface brightness calculated by assuming the fluxes listed above are uniformly distributed throughout the beam sizes quoted in the reference papers. The green and red lines are the respective sensitivity and saturation limits for each instrument. The sensitivity values used are for a 5 sigma detection of an extended source with a 500 second exposure.

Infrared images

DSS 2nd Generation Red (Search the DSS)

2MASS K band (Search the 2MASS Quicklook Image Server)

ISO-CAM 7.7 microns (Search the ISO archive)

5 degree IRAS 12 micron image centered on M57 ( Retrieve IRAS images using OASIS)

ISO-CAM 14.9 microns (Search the ISO archive)

5 degree IRAS 100 micron image centered on M57 ( Retrieve IRAS images using OASIS)

Infrared Spectra

click on image for full 2 to 40 micron spectra with ISO-SWS (Search the ISO archive)

click on image for full 40 to 200 micron spectra with ISO-LWS (Search the ISO archive)

Spitzer Observations

• This object is part of GTO programs to study stellar ejecta and dust formation with IRAC and MIPS. (Program ID numbers 68 and 77)
  (You can download the AORs (Astronomical Observation Requests) for this object into Spot by using "View Program" under the "File" menu and entering these program IDs.)
• Search the ROC for planned observations

Further reading

• ISO LWS observations of planetary nebula fine-structure lines, Liu, X.-W., Barlow, M. J., Cohen, M., Danziger, I. J., Luo, S.-G., Baluteau, J. P., Cox, P., Emery, R. J., Lim, T., Péquignot, D., 2001, MNRAS, 323, 343.
• Low-excitation atomic gas around evolved stars. I. ISO observations of C-rich nebulae, Fong, D., Meixner, M., Castro-Carrizo, A., Bujarrabal, V., Latter, W. B., Tielens, A. G. G. M., Kelly, D. M., Sutton, E. C., 2001, A&A, 367, 652.
• Low-excitation atomic gas around evolved stars. II. ISO observations of O-rich nebulae, Castro-Carrizo, A., Bujarrabal, V., Fong, D., Meixner, M., Tielens, A. G. G. M., Latter, W. B., Barlow, M. J., 2001, A&A, 367, 674.
• Mid-infrared spectral images of planetary nebulae with ISOCAM, Persi, P., Cesarsky, D., Marenzi, A. R., Preite-Martinez, A., Rouan, D., Siebenmorgen, R., Lacombe, F., Tiphene, D., 1999, A&A, 351, 201.