Saao Standards For Optical Photometry

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UBV I Surface Photometry of the Spiral Galaxy NGC 300 in

system using the equatorial standards of South African Astronomical Observatory (SAAO) (Menzies et al. 1991) and blue and red standards of Kilkenny et al. (1998), both observed on the same night. The atmospheric extinction coefficients were determined from the photometry

Dave Kilkenny -

Another two examples of the results of di erential photometry are shown. These are both pul-sating Hydrogen{de cient stars (sometimes called Helium stars, or Extreme Helium (EHe) stars) with very short periods (near 0.1 day). Figure 3: Light curves for (upper) LSS 3184 (BX Cir) and (lower) V652 Her. The upper data are from several

arXiv:astro-ph/9707324v1 29 Jul 1997

Even with excellent local standards and image quality, there can be systematic differences as large as δ(m) WFPC2 optical photometry was measured by P. Challis, SAAO, and LCO photoelectric photometry. I also include the photoelectric data published by Matthews (1987),

Combined Optical and Near-IR IRAC2 Photometry of the Bulge

Eight SAAO standards (kindly provided by Dr. Ian Glass) were observed during the run and most of them on at least two positions of the array. The calibration curve and all the details regarding the standard stars have already beenpub- lished in Ferraro et al., 1993. The optical BVRl sample, coming from Ortolani, Barbuy and Bica (1990), has

Open Research Online

Optical spectroscopic observations were made with the 1.9 m telescope at the South African Astronomical Observatory (SAAO) on 1997 June 23, the 1.3 m tele-scope at Mount Skinakas (Crete, Greece) on 1999 July 27 and 2000 July 20{22 and the ESO 1.52-m telescope at La Silla Observatory, Chile on 2000 September 13. The


obtained optical spectra of V347 Pup using the Cassegrain spectrograph + SITe1 CCD chip on the SAAO 1.9-m tele-scope. Simultaneous photometry was available for most of the spectra using the SAAO 1.0-m telescope with the TEK8 CCD chip. See Table 1 and its caption for full details. On the December 1998 run, we observed 17 spectral

arXiv:astro-ph/0307373v1 21 Jul 2003

The optical spectrum is that of a typical LMXB with weak Hα, Hβand HeII λ4686 emission superimposed on a blue continuum. The characteristics of the optical spectrum, the relatively soft X-ray spectrum, and the high X-ray to optical luminosity (LX/Lopt ∼ 600), imply LMC X 2 is sim-ilar to galactic LMXBs (e.g. van Paradijs 1983). The optical

Correlation study of multi-wavelength transient emission

optical observations will include photometric observations with the UFS/Boyden 1.5-m telescope at the Boyden Observatory and spectroscopic observations with the SAAO 1.9-m telescope, using Landolt photometric standards. Aperture photometry is not the ideal photometric process

On the nature of the variable star UNSW-V-760

time series photometry. A spectroscopic classification is derived in Section 5. The interpretation of all the available data is discussed in Section 6 and the paper concluded in Section 7. 2 PHOTOMETRIC OBSERVATIONS AND REDUCTIONS Observations were made with the South African Astronomical Ob-servatory (SAAO) CCD cameras mounted on the SAAO 1.0-m tele-

Observing Supernovae in the Infrared

IR Photometry Generally similar to optical, with a few caveats Sensitive to changes in humidity. Observe stds. often. Keep track of humidity In principle, can be included in photometric soln. Stay Linear! Shallow wells. Check pre-subtracted images.

RoboPol: optical polarimetry in Crete - Polarisation

Photometry Optical: Jonhson, Strömgren and interference filters (OII, OIII, SII, NII, Hα, etc) Infrared (J, H, K) and a set of narrow band filters (FeII 1644, H-2 2122, H-2 2144, BrG 2166, CO 2295) Spectroscopy Set of gratings providing spectral resolution R=1000-8000 Polarimetry RoboPol photopolarimeter (BVRI)

Irregular variables of type Lb. - A&A journal

New JHKL0M-photometry for 160 stars? F. Kerschbaum1, C. Lazaro2;3 and P. Habison1 1 Institut f¨ur Astronomie der Universit¨at Wien, T¨urkenschanzstraˇe 17, A-1180 Wien, Austria 2 Dpto. de Astrof sica, Fac. de F sica, Universidad de La Laguna, 38200-La Laguna, Tenerife, Spain 3 Instituto de Astrof sica de Canarias, 38200-La Laguna, Tenerife

SA University of ASSA 7 Aug

SALTICAM (optical imager) Facility instruments: Acquisition camera (SALTICAM) Guidance & focus system PFIS slit-viewing optics Fold mirrors (to 3 focii) Moving pupil baffle Atmospheric Dispersion Compensator (ADC) SAC structure Payload alignment system (autocollimator and interferometer) Calibration system (flats, arcs)


Standards from andLandolt (1992), Bessell (1990), been the SAAO system, but in fact et al.Kilkenny (1997) have shown that the Bessell (1990) 2 IRAF is distributed by the National Optical Astronomy Obser-vatories, which are operated by the Association of Universities for

Outflows and Disks around Young Stars: Synergies for the

as Essential Standards. Optical Photometry LCOGT u Vi SAAO, DFOT, AZT -11/FLI PL -230, Thai National telescopes, Catania 0.91m, McDonald, and other small telescopes. Outflows and Disks around Young Stars: Synergies

monthly notes of the astronomical society of southern africa

Na onal Measuring Standards (NMS) of Mass, Pressure and Length. During the 1950s Roy became a familiar face at the Radcliffe Observatory through ASSA mee ngs. He used to store his 10-inch telescope (mirror made and signed, Calver 02 ) in Mike Feast s garden. The Director of Radcliffe Observatory, Dr Andrew D Thackeray, asked if he would


2. Photometry 2.1. Photometric standards and calibration Work on photometric standards and calibration, which underpins all photometric appli-cations, proceeded during the triennium under review. Many issues of standardization were discussed in the conference reviewed in

UBVI CCD photometry of M11 ± II. New photometry and

Extensive UBVI CCD photometry has been obtained for the intermediate-age open cluster M11 (NGC 6705). From this new photometry we derive the cluster parameters ‰V0 2 MV ˆ 11:55 ^0:10; E B 2V†ˆ0:428^ 0:027 and radius ˆ 16arcmin] and age logtage ˆ 8:4 ^0:1†: We also derive density profiles and confirm the mass segregation in M11. The

ASTRONOMY AND Time-resolved HST and IUE UV spectroscopy

2.3. The optical photometry Optical photometry was conducted in the period October 18 231995 at the SAAO 0.75m telescope and UCT Photometer employing a Hamamatsu R93402 GaAs photomultiplier. BVRI (Cousins) photometry was carried out on the first three nights performingsymmetricmoduleswithintegrationtimesof30sor

The component masses of the cataclysmic variable V347 Puppis

We present time-resolved spectroscopy and photometry of the double-lined eclipsing cata-clysmic variable V347 Pup (=LB 1800). There is evidence of irradiation on the inner hemi-sphere of the secondary star, which we correct for using a model to give a secondary-star radial velocity of KR = 198 ± 5kms−1.

University of Cape Town - OpenUCT Home

The accuracy of infrared photometry has not hitherto been comparable to that mhich is achievable in visual region photometry but the need for the best possible set of standards is obvious. A first attempt to set up a reliable set of southern infrared standards was made by Glass (1974).

Infrared array photometry of bulge globular clusters

Eight SAAO standards (kindly provided by Dr. Ian Glass andthenpublishedon1995byCarter)wereobservedduringthe run and most of them at two positions of the array, at least. The calibration curve and details regarding the standard stars were presentedinFerraroetal.(1994).Theadoptedcalibrationequa-tions linking the instrumental photometry to the Carter/SAAO

An Introduction - Energy Research Centre (UCT)

South African Astronomical Observatory (SAAO), Cape Town March 19 th, 2009. About this presentation What s a Virtual Observatory? First, a real observatory-Telescope (optical, infrared, ultra-violet, radio, x-ray) Detectors, instruments (cameras, spectrographs, photometers) Site (ground, space) Metadata standards


3/6/2015  the poor X-ray location, lack of optical counterpart and very different X-ray properties make the association of Cen X-2 with BW Cir disputable. Dynamical evidence for a BH in BW Cir was first presented in Casares et al. (2004, C04 hereafter). Spectroscopic features of a G0-5 III donor are shown to move in a 2.5 days orbital period.

JHK standard stars for large telescopes: the UKIRT

nomical Observatory (SAAO) system of Glass (1974) is most recently manifest in the work of Carter (1990) and Carter & Meadows (1995). The Anglo-Australian Observatory (AAO) system (Allen & Cragg 1983) derives from this and more especiallyfromtheMountStromloObservatory(MSO)system(cf. Jones & Hyland 1982), of which a more recent descendant is the


THE OPEN CLUSTER NGC 2516. I. OPTICAL PHOTOMETRY HwankyungSung AstronomyProgram,SchoolofEarthandEnvironmentalSciences,SeoulNationalUniversity,Seoul151-742,Korea;[email protected] MichaelS.Bessell ResearchSchoolofAstronomyandAstrophysics,AustralianNationalUniversity,PrivateBag,WestonCreekPO,ACT2611,Australia;

Spectroscopic characterization of galaxy clusters in RCS-1

optical searches for overdensities of galaxies (Abell 1958). In re-cent years, colour-based variations (e.g. Gal et al. 2000; Gladders E-mail: [email protected] &Yee2000; Miller et al. 2005) of Abell s original method have led to decreased false positive rates from unrelated line-of-sight projections of clusters, and high completenesses.


formations for stars of extreme color. The SAAO CCD system, filters, and color equations are discussed in detail by Walker (1984). This equipment has well-known pho-tometric properties and has been shown to be capable of accurately reproducing the UBV system. The CTIO 4-m observations are summarized in Table I. The standards

arXiv:2012.08534v1 [astro-ph.CO] 15 Dec 2020

2 Riessetal. 1. INTRODUCTION This is the second paper in a series reporting on efforts to improve knowledge of the distance scale and the Hubble constant (H0) by combining parallax measurements of Milky Way (MW) Cepheids from the ESA Gaia mission (Gaia Collaboration et al. 2016a,b, 2018) and multi-band photometry of

Improved SAAO 2MASS photometry transformations

2South African Astronomical Observatory, PO Box 9, Observatory, 7935 Cape, South Africa Accepted 2007 June 12. Received 2007 June 6; in original form 2007 March 12 ABSTRACT Near-infrared photometry of 599 stars is used to calculate transformations from the South African Astronomical Observatory (SAAO) JHK system to the Two-Micron All-Sky Survey (2MASS) JHK

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Differential photometry was performed using the Univer-sity of Cape Town (UCT) CCD (O Donoghue 1995) and the new Sutherland High-speed Optical Cameras (SHOC; Gulbis et al. 2011a, Coppejans et al. 2013) mounted on the 74-in and 40-in reflector telescopes of the South African As-tronomical Observatory (SAAO).

Standard Stars: CCD Photometry, Transformations and

star photometry was performed by Dr A. W. J. Cousins. Astronomers at the South African Astronomical Obser-vatory (SAAO) continue to refine the accuracy (Menzies et al. 1989) and to extend the colour range (Kilkenny et al. 1998) of the standards. Although E-regions provide the most accurate standards available currently, there are several limitations.


superhumps in cataclysmic binaries. xxiii. v442 ophiuchi and rx j1643.7+3402 joseph patterson, 1,2 william h. fenton, 3 john r. thorstensen, 3 david a. harvey, 4 david r. skillman, 5 robert e. fried, 6 berto monard, 7 darragh o'donoghue, 8 edward beshore, 9 brian martin, 10 panos niarchos, 11 tonny vanmunster, 12 jerry foote, 13 greg bolt, 14 robert rea, 15 lewis m. cook, 16 neil butterworth,

Are the Bulge C stars in the Sagittarius dwarf galaxy?

tudes from the standards observed at ESO in the period 1983 1989. The near-IR photometry from WIC96 with the SAAO 1.9m telescope is appropriately transformed to the ESO system (Hron et al. 1997). Note, that in general many transformations from SAAO to the ESO near-IR system refer to the transformation from the system defined by Fig. 1.

MNRAS 429, 652 660 (2013) doi:10.1093/mnras/sts370

The bulk of the observations were made with the South African Astronomical Observatory (SAAO) STE4 CCD camera, mounted on the SAAO 1.9 m telescope at Sutherland, South Africa. The camera is equipped with 1K × 1K chip, giving a field of view of about 2.5arcmin×2.5 arcmin. All observations were pre-binned

Concept of SPARC4: A Simultaneous Polarimeter and Rapid

HIPPO6 is a two-channel optical imager with polarimetric capability. The bands are selected by a chopping filter wheel and the detectors are photomultiplier tubes. It is used at the 1.9-m telescope of the South African Astronomical Observatory (SAAO). RINGO27 is a polarimeter installed at the 2.0-m Liverpool Telescope, a fully robotic

BVRI Photometry of the ω Centauri Hubble Space Telescope

ing the photometry for the local standards. It was found that the mean zero point for the faintest four local standards showed shifts of only (A V,A£- V,A V-RyA V-/) = (0.000, 0.002, 0.009, 0.013) mag between the two observing runs, giving confidence in the accuracy of the photometry. The magnitudes of the local standards were then adjusted to the


Baltic Astronomy, vol.21, 271{297, 2012 L3 Dynamics and Poincar e Maps in the Restricted Full Three Body Problem Pauli Pihajoki1;2, Elisabet Herrera-Sucarrat2, Phil Palmer2 and Mark Roberts3 1 Tuorla observatory, Department of Physics and Astronomy, University of Turku, V ais alantie 20, FI-21400 Piikki o, Finland; [email protected] 2 Surrey Space Centre, Department of Electronic Engineering

Northern JHK Standard Stars for Array Detectors

the UKIRT list of faint standards those stars with declinations ≥ 0 and with K magnitudes & 8.5; J−K colors for this subset range from −0.2 to 0.6. The UKIRT list comprises optical standards from selected areas (Landolt 1983), HST calibration objects (Turnshek et al. 1990), and stars in M67 (Eggen & Sandage 1964) and in the globular clus-


tronomical Observatory (SAAO) with a 1 m telescope and a 1k×1kSITecharge-coupleddevice(CCD)atSAAObetween 2007 February 21 27 and 2007 May 2 8. The SITe CCD has afieldofviewof26arcmin2 at the f/16 Cassegrain focus of the 1 m telescope. Of the 30 40 other stars recorded per field, several bright stars were used as local differential standards. 2