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Image smearing caused by CTI in a Hubble Space Telescope image

Image smearing caused by CTI in a Hubble Space Telescope image


Image smearing caused by CTI in a Hubble Space Telescope image shown as the raw image (left) and after image correction has been applied (right).


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New data from the Hubble Space Telescope and computer simulations have revealed that the universe has much less ultraviolet light than previously thought.

he European Space Agency's Planck space telescope mapped the cosmic microwave background. Credit: ESA and the Planck Collaboration

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Figure 7.

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Night Facility

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These views are from the approach of Juno at Jupiter during on May NASA/Juno Mission. Image processing by Sean Doran.

The Enoch Pratt Library - GovansIn 1919 Glenn Perine helped another cause in his neighborhood (other than the Chapel at Redeemer) - a library for Gova.

The Homeland Wolf

This infrared image of Saturn's largest moon, Titan, was one of the first produced by the SPHERE instrument soon after it was installed on ESO's Very Large ...

An amazing shot of the heavens also says something of humanity. Spiral GalaxyTelescope ImagesHubble Space ...

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Academy Award winner Morgan Freeman narrates an episode of Through the Wormhole, a Science Channel

When cosmic rays (CRs)—high-energy protons, neutrons, and ions—impact CCDs, they frequently displace photoelectrons, causing the familiar trails ...

Figure 7.

This image from NASA's Swift space telescope, taken on Jan. 22, 2014, shows the supernova SN 2014J as seen in three different exposures by the space ...

Saturn's Double Light Show - Credit: NASA, ESA, and Jonathan Nichols (University. Hubble Space TelescopeTelescope ...

SETI Institute's Allen Telescope Array

CSIRO Parkes Observatory

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Comparison between the Cramér–Rao bound in the presence of radiation damage (dotted lines

Fig. 4.— Covariance matrix for the 2D correlation functions C 1 ()

—Contribution functions for all six wavelengths after 25 iterations

This ...

The BRITE Constellation Nanosatellite Mission: Testing, Commissioning, and Operations - IOPscience

The simulation process: (top left) optical PSF, (top right) pointing

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Figure 4. Left: Presented are our Hβ+[OIII] Luminosity Functions along

The next image shows CTA 102, marked by the two white lines. Incidentally, note also the faint galaxy NGC7305, a small round smudge to its lower left.

Top panel: comparison between the observed CTI-free observations {{Nk}}

Gemini South telescope

NASA's Hubble Space Telescope captures a rare view of the entire ring system of the planet

... composite image containing x-rays from NASA's Chandra X-ray Observatory (red) and optical data from the Hubble Space Telescope (pink, yellow, and blue).

Figure 2. An example of what is so intriguing about Eta Car: the extended

Logarithmic space density functions for the most probable RC stars in the fields

Comparison between the image flux estimation bias (in units of magnitude) before (top

Location bias after a CTI mitigation using the LSF model , representative of an ideally calibrated

Comparison between the Cramér–Rao bound in the presence of radiation damage (dotted lines

Image location bias recovery using the CTI-mitigation forward-modelling approach including the current

Image location standard errors resulting from the use of the CTI-mitigation forward-modelling

Fig. 9. Observed (left) and de-reddened (right) colour

Figure 34.

CTI Effects Models for GAia (CEMGA) Monte Carlo simulations at

Figure 3. Left: Results of on-ground experiments carried out in order to

Fig. 7. Normalized contribution functions showing the location of the line formation regions of

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Figure 10. Cumulative clump luminosity functions. The z = 0 data are from the

[Gotta give props to my alma mater]

HIghMass-High H I Mass, H I-rich Galaxies at z ~ 0 Sample Definition, Optical and Hα Imaging, and Star Formation Properties

Figure 1. Six OB stars of NGC 2244 embedded in the central cavity of the

Fig. 1. ACS color image of Abell 1703 (combination of the HST filters

Figure 33.

Diffracto-Astrometry Measurements: Accuracy of the Measuring Algorithm

Figure 1. Example of three independent noise realisations of our simulated image of a faint

Fig. 1. Skymap of total integrated flux over the Milky Way, in the

Diffracto-Astrometry Measurements: Accuracy of the Measuring Algorithm

CFHTLenS: Weak lensing constraints on the ellipticity of galaxy-scale matter haloes and the galaxy-halo misalignment

Fig. 24.—

NGC 1999, bright reflection nebula in Orion. - Stock Image

Fig. 7.—Contribution functions ð@ [email protected] ln uÞð@B =

Figure 1. Deep optical images of a sub-sample of nearby Early-Type

Inferred H{\alpha} Flux as a Star-Formation Rate Indicator at z ~ 4-5: Implications for Dust Properties, Burstiness, and the z = 4-8 Star-Formation-Rate ...

Just weeks after NASA astronauts repaired the Hubble Space Telescope in December 1999, the Hubble

California Nebula by Konstantin Mironov - Pixdaus

Fig. 3. Silvaco pixel model-simulated AC electron density profiles through different sized

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Figure 3. Normalized contribution functions for retrieval of Titan's pressure/ temperature profiles from CH


Fig. 5.—Contribution functions ð@B [email protected] Þð@ =

Figure 15. Cumulative functions of the star formation histories shown in Figure 14, showing

Figure 7. In the low signal-to-trap regime, approximations made to

(PDF) The XMM Cluster Survey: The Build-up of Stellar Mass in Brightest Cluster Galaxies at High Redshift

Capturing Jupiter's moons is easy enough, and Sky and Telescope's excellent javascript utility can help you identify the moons.

Figure 4.

Fig. 1.— NGC 4449 and its halo stream. Left: image from

Fig. 1.— Color image from F475W, F625W, and F775W observations.

Fig. 1.— Left: FUV image (taken in SBC/F140LP)

(PDF) Velocity Segregation and Systematic Biases In Velocity Dispersion Estimates With the SPT-GMOS Spectroscopic Survey

White-chinned petrel (Procellaria acquinoctialis) flying in a ray of light, Ile

The historical feelings were present anyway, since this object was discovered by Milton Humason from that same telescope !


One of the first images from the Dark Energy Camera, showing the spiral galaxy NGC

Serial CTI measured as a function of temperature

Fig. 4. False colour (K S =blue, WISE W2=green,

Fig. 2 tn vs r using different functions. The blue curve for tn =

Figure 1.

Measurement of the Cold Dark Matter-Neutrino Dipole in the TianNu Simulation

Fig. 10.—Uncertainties of the beam transform functions for all bands. The

Fig. 2.— The ratio of kinetic to radiated energy in 58 nova models