Once students get the hang of it, they can find and measure the brightness of Delta Cephei in a few minutes. ... of Delta Cephei . ... Oct. ... The following table lists the measurements of Delta Cephei made by one amateur astronomer in autumn 1990. ... 4.0 . ... This activity is a simplified version of one that appeared in Hands-On Astrophysics, a series of activities prepared by the American Association of Variable Star Observers with support from the National Science Foundation. << previous page | ...

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• ASP: Using Multicultural Dimensions to Teach Astronomy

... About ATNF overview . ... Australia Telescope Steering Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . ... Australia Telescope 20GHz Survey . ... Bright prospects: Comparing the H Survey with large-scale radio continuum emission . ... Prospects for comparisons between the AAO/UKST H \ survey and large-scale radio continuum emission are considered, with particular reference to the recently completed Parkes 2.4-GHz survey of the southern Galactic Plane. ...

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• PhD Thesis Abstract
• ATCA_mm_science
• PPTA Wiki | Observing / Details

... The concerns here are similar to those for observing bright targets; saturation and blooming of the bright companion PSF must not impact the faint target. Also, one may need to consider subtracting the PSF of the bright object, and effects which limit the accuracy of that subtraction. If the bright companion will saturate and bloom, it will be necessary to rotate the CCD so that blooming along the CCD columns does not obliterate the faint target. ...

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• A multi-scale study of infrared and radio emission from Scd galaxy M 33
• Terrestrial Silicates Compared to Astronomical Silicates
• WFPC2 Instrument Handbook Update

... A detailed study of two consecutive bright points observed simultaneously with CDS, EIT and MDI is presented. The analysis of the evolution of the photospheric magnetic features and their coronal counterpart shows that there is a linear dependence between the EIT Fe XII 195? flux and the total magnetic flux of the photospheric bipolarity. ... In a follow-up study, we used wide slit (90arcsec240arcsec) movies of four EIT coronal bright points (BPs) obtained with CDS. ...

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• Explosive Events
• Observations with the Faulkes Telescopes
• Observations with the Faulkes Telescope North

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

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• A collection of images
• K-band Arcetri Obscured Supernova Search - Detected Supernovae
• The puzzling core of the Phoenix cluster: deep X-ray observations

... 205Anglada+ 0) and NH3(1,1) observations towards 172 different star forming regions (99 observed in both molecules) associated with H2O maser emission. We make a comparative study between the physical parameters obtained from the CS and NH3 spectra, and their relationship with the H2O maser emission. ... We find that both the CS and the NH3 lines are significantly wider in regions with H2O masers than in other regions. ...

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• Using the sky model
• The sample description
• Optical spectroscopy

... The bright supernova (hereafter SN) in the galaxy NGC 4527 was first sighted by S. Knight (USA) on April 13.17UT at magnitude ~14.0v. The report of the sighting was subsequently forwarded by phone to the AAVSO. ... SN 1991T. The galaxy NGC 4527 is an Sb(s)II type galaxy with an apparent Blue magnitude of 11.32 (Shapley-Ames, 1981). ... An analysis of this event utilizing visual observations by amateurs, plus a light curve is presented.. ... THE LIGHT CURVE: . ... ISN SN 1991T web page . ...

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• SN1989B in M66

... Here are some general thoughts about the role of Mark5 recording in pulsar experiments. Pulsar work with the Mark5 Backend: Advantages: Flexibility: Set frequency time resolution after observations, enabling multiple analyses of the data. ... We can use the Mark5 recorders to gauge stability of the other pulsar timing backends: at multiple telescopes, and multiple epochs). ... The properties of these features changes as the scattering medium changes on day-month time scales. ...

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• Solar System Studies at AO
• I-GALFA Infrared Emission
• NAIC-NRAO Single Dish Summer School 2005 NAIC-NRAO Single Dish Summer School

... Observing . ... Solar Observing . ... April 3 (SUN) - Solar Observing, Central Park , Manhattan . ... APRIL'S SKY . ... Lecture Series at the American Museum of Natural History The Amateur Astronomers Association is proud to present an astronomy lecture series from October through May each year for our members and the .. ... The€аAmateur Astronomers Association of New York€аwas organized in 1927 to promote the study of Astronomy, emphasizing its cultural and inspirational value. ...

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• Lecture Series 2015-2016 ? Amateur Astronomers Association of New York
• Brooklyn Museum Plaza ? Amateur Astronomers Association of New York
• Astronomy Workshop: Observing Variable Stars from the City ? February 15, 2015

Emission Line Diagnostics in a ``No UV Bump'' Quasar PHL909 Smita Mathur, Belinda Wilkes, Martin Elvis and Jonathan McDowell Abstract PHL909 is a quasar with unusually low ultraviolet luminosity (blue bump strength C UV=IR = \Gamma0:20 compared to an average value of 0:4 (McDowell et al. ... The intrinsic continuum of PHL909 ( i.e. as seen by the BELR ) may thus be similar to the `standard' continuum, with a big blue bump, reddened along the line of sight. ...

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• Very Low Mass PMS Objects
• Spectroscopic Data
• Period Criteria

... In order to compare the number of different evolutionary stages obtained and X-ray luminosity of the chosen X-ray sources with the observed galactic values we use the sum of C/O+O/C , where C and O are the calculated and observed values of a given binary type, respectively. If we make comparison for a number of different binary species (for example, we compare the number of CV, number of X-ray pulsars,   total X-ray luminosity of LMXB, etc.), we write this criterion in the form: . ...

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• Discussion and conclusions

... Flux density at 1 GHz (/Jy): 250 . ... Radio: Distorted shell, brighter to the E, with pulsar and associated nebula. ... ADS . ... Molonglo at 408 MHz (3': S=299 Jy). ... Einstein observations. ... 1991, ApJ, 372, L99. ... VLA at 327 MHz (3'.6?3'.8: S=469 Jy). ... VLA at 1.4 GHz (15''), plus X-ray spectra. ... 1996, ApJ, 461, 820. ... VLA at 1.5 and 8.4 GHz (8".9?7".8) of pulsar nebula. ... Reach & Rho 1996, A&A, 315, L277. ... VLA at 74 MHz (36''?39'': S=634?70 Jy) and 324 MHz (13'': S=411?50 Jy). ...

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• G349.7+0.2
• CO in NGC 1530, aperture synthesis of a barred spiral
• G315.4-2.3

... The following charts/text are intended as tools for monitoring the Type Ia supernovae ( SNe ) event visually or photographically (utilizing telescope equipped CCD equipment).The files include: A replication of The Type Ia SNe , V- magnitude (with data point checks from other cited references)and color index (B-V) templete (to indicate a general color-related trend of the type Ia ... I believe this might help alleviate some of the problems involving the making of acceptable amateur light curves...

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• SN 1989B Light Curve Analysis.
• APOD Index - Dark Matter
• APOD: 2002 October 11 - Fomalhaut Dust Disk Indicates Planets

... Contacts . 2012: . ... We refined the fundamental parameters of the components, the orbital periods, and the conditions of photospheric heating of the secondary component by the ultraviolet radiation of the hot component. ... The observations of the star clusters associated with ultra-luminous x-ray sources (ULXs) in four galaxies on the 6-meter and VLT telescopes have shown that all the ULXs are located within 200pc of very young star clusters (younger than 5 million years). ... Archive . ...

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• Lack of Dwarf Galaxies in the Local Volume Compared to Conventional Cosmology
• Detection of unique bright radio flare of X-ray binary
• Solar system sector, archive 1994

Peremennye Zvezdy ( Variable Stars ) 33 , No. ... The new variable star HD 305629, with a Cepheid-like light curve, is demonstrated, from our optical observations and ASAS-3 data, to actually be an ellipsoidal variable star on a highly eccentric orbit. ... During a systematic search of variable stars in the publicly available ASAS-3 database (Pojmanski 2002), apparent variability was found in the star HD 305629 (10 51 34 35, -60 47 57 4, J2000.0; Fig. ... The light curve and color curves of HD 305629. ...

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• XWare > APOD

The problem of solar wind data correlation for the observations onboard several spacecraft is very important for three points of view: . ... This problem is studied now in detail by systematic determination of ion flux and ion velocity data correlations by INTERBALL-1 (IKI group), WIND and IMP 8 (both - MIT group). ... Solar wind plasma correlation lengths from IMP 8, WIND and INTERBALL-1. ... Correlation of solar wind observations onboard several spacecraft: INTERBALL-1, IMP 8 and WIND data. ...

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• Цикл работ на конкурс статей
• Solar Energetic Particles
• Main results of the experimental and theoretical research completed in 2010

... It provides long range planning information to the scheduling team; it provides bright object, timing, and orientation information to the observation planning team; and it provides graphical description of the observations and their constraints. ... The GUI graphically displays the constraints that are computed by Spike and stored in the description files and in the database. ... BOAS processes all bright objects that have entered the database since the last time BOAS was run. ...

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• NICMOS Software: An Observation Case Study
• Asteroseismology-Observing for a SONG
• Prototypical Operations Support Tools for NASA Interferometer Missions:

... Paul Bennie pbe@star.le.ac.uk Friday, 16 February 2001 XMM EPIC MOS MOS-2 pixels. ... Paul Bennie pbe@star.le.ac.uk Friday, 16 February 2001 The defect seem to be most quick CCDs 1, 2 XMM EPIC MOS MOS-1 pixels. ... Paul Bennie pbe@star.le.ac.uk Friday, 16 February 2001 XMM EPIC MOS New Defects in rev. 108 flare. XMM EPIC MOS Paul Bennie pbe@star.le.ac.uk Friday, 16 February 2001 New Defects in rev. 169 flare. ... Paul Bennie pbe@star.le.ac.uk Friday, 16 February 2001 XMM EPIC MOS ...

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• How to extract MOS spectra of a point-like source and associated matrices
• XMM-Newton OM Response Files Page
• How to extract PN spectra of a point-like source and associated matrices

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

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• http://www.gao.spb.ru/english/publ-s/viii-rfs/p091.pdf
• Pulkovo NEO Page: Estimation of Accuracy of the Observations

... Star Atlas . ... Scientists find "fluffy" disk around baby star . ... The team's analysis of the disk shows that a "fluffy" layer above it is responsible for the scattered light observed in the infrared image. ... HiCIAO uses a mask to block out the light of the central star, which may be a million times brighter than its disk. ... This type of observation is preferred for faint emissions associated with scattered light around planet-forming disks, as there is less light from the much brighter star....

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• Bright planets meet at dusk | Astronomy.com
• What are typical star-to-star distances in globular clusters compared to
• Observations of optical flares challenge theories on magnetars | Astronomy.com