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Planck nos acerca al primer acto de la formación del Universo

11 enero 2011

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This animation illustrates the position on the sky of all compact sources detected by Planck during its first all-sky survey and listed in the Early Release Compact Source Catalogue (ERCSC). It shows how they compare to the microwave view of the sky, also seen by Planck.

The ERCSC contains more than 15 000 compact sources and comprises a wide variety of astronomical objects, both galactic (including cold molecular cloud cores and stars with dust shells) and extragalactic (such as radio galaxies, blazars, infrared-luminous galaxies and galaxy clusters). It represents a rich and robust database for the entire astronomical community.

The size of the spots displayed in the series of images reflects the brightness of the sources.

Credits: ESA/Planck Collaboration

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first six fields used to detect Cosmic Infrared

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This image shows the location of the first six fields used to detect and study the Cosmic Infrared Background. The fields, named N1, AG, SP, LH2, Boötes 1 and Boötes 2, respectively, are all located at a relatively high galactic latitude, where the foreground contamination due to the Milky Way's diffuse emission is less dramatic.

Credits: ESA/Planck Collaboration

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This animation shows the network of clumped structures corresponding to the distribution of dusty, star-forming galaxies on very large scales and throughout cosmic history. The various frequencies probed by Planck's HFI instrument reveal different amounts of structure. This is because each frequency is most sensitive to emission coming from galaxies at certain distances. Hence they show the progress of galaxy formation.

Observations at the highest frequency, 857 GHz, yield the most information about the closer galaxies, whereas the lower frequencies offer a chance to peer farther and farther away, emphasising Planck's ability to track down the early phases of galaxy formation.

The patch of the sky shown in this animation is located at relatively high galactic latitude, where the foreground contamination due to the Milky Way's diffuse emission is less dramatic.

Credits: ESA/Planck Collaboration

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The colour composite of the Rho Ophiuchus molecular cloud highlights the correlation between the anomalous microwave emission, most likely due to miniature spinning dust grains observed at 30 GHz (shown here in red), and the thermal dust emission, observed at 857 GHz (shown here in green). The complex structure of knots and filaments, visible in this cloud of gas and dust, represents striking evidence for the ongoing processes of star formation.

The composite image (right) is based on three individual maps (left) taken at 0.4 GHz from Haslam et al. (1982) and at 30 GHz and 857 GHz by Planck, respectively. The size of the image is about 5 degrees on a side, which is about 10 times the apparent diameter of the full Moon.

Credits: ESA/Planck Collaboration

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This image shows one of the newly discovered superclusters of galaxies, PLCK G214.6+37.0, detected by Planck and confirmed by XMM-Newton. This is the first supercluster to be discovered through its Sunyaev-Zel'dovich effect. The effect is the name for the cluster’s silhouette against the cosmic microwave background radiation. Combined with other observations, the Sunyaev-Zel'dovich effect allows astronomers to measure properties such as the temperature and density of the cluster’s hot gas where the galaxies are embedded. The right panel shows the X-ray image of the supercluster obtained with XMM-Newton, which reveals that three galaxy clusters comprise this supercluster. The bright orange blob in the left panel shows the Sunyaev-Zel'dovich image of the supercluster, obtained by Planck. The X-ray contours are also superimposed on the Planck image.

Credits: ESA/Planck Collaboration; XMM-Newton image: ESA

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