scholarly journals The La Palma Data Archive

1989 ◽  
Vol 110 ◽  
pp. 139-140
Author(s):  
Chris Benn
Keyword(s):  
Data Archive ◽  
Isaac Newton ◽  
La Palma ◽  
Data Archives ◽  
International Ultraviolet Explorer ◽  
Isaac Newton Telescope ◽  
The Republic ◽  
Volcanic Caldera ◽  
The Uk ◽  
William Herschel

The Observatorio del Roque de los Muchachos is perched atop a volcanic caldera on the island of La Palma in the Canary Islands, 400 km off the coast of North Africa. Three of the telescopes at the observatory are products of a collaboration between the UK, the Netherlands, Spain and the Republic of Ireland. They are the 1.0-m Jacobus Kapteyn Telescope, the 2.5-m Isaac Newton Telescope and the 4.2-m William Herschel Telescope (which saw first light in July 1987)1. The telescopes are computer controlled (running under ADAM software), and the observations are recorded primarily in electronic form. Recognising the success of astronomical-satellite data archives, such as that generated by the International Ultraviolet Explorer, a La Palma Data Archive has been established at the Royal Greenwich Observatory. The archive will be used by astronomers wishing to exploit data obtained by other observers, by engineers interested in the performance of telescope and instruments under varying conditions, and for monitoring the way in which the telescope is used.

scholarly journals Galaxy Number-Counts to B = 28M

1994 ◽  
Vol 161 ◽  
pp. 645-648
Author(s):  
N. Metcalfe ◽  
T. Shanks ◽  
N. Roche ◽  
R. Fong
Keyword(s):  
Power Law Distribution ◽  
Isaac Newton ◽  
La Palma ◽  
The Galaxy ◽  
History Of ◽  
Isaac Newton Telescope ◽  
William Herschel ◽  
Ccd Detectors ◽  
Number Counts ◽  
Evolving Models

Counting the number of galaxies as a function of their apparent brightness is one of the fundamental cosmological tests, providing an important probe of both the geometry and evolutionary history of the Universe. CCD detectors have in recent years enabled astronomers to explore magnitude limits undreamed of a decade or so ago, and where important constraints can be placed on the allowable combinations of q 0 and evolution. Recent work has shown that the B-band counts keep rising with a power-law distribution, with a fivefold excess in the number of galaxies at B = 26.5 over that expected from simple non-evolving models. Indeed, it has been suggested that the total numbers of galaxies already seen may be too high for a q 0 = 0.5 universe, assuming there is a redshift cut-off in the galaxy distribution caused either by galaxies having strong Lyman limit systems or a low redshift of formation. As q 0 = 0.5 is favoured by theoretical arguments, it is important to see if the behaviour of the counts at even fainter magnitudes can be reconciled with a high density universe. Most published counts are unreliable faintward of B ≈ 26, as the incompleteness corrections required become comparable in size to the data. We have now extended the counts to B ∼ 28, using a ∼ 24 hour CCD exposure taken on the 2.5 m Isaac Newton telescope (INT) on La Palma, together with a ∼ 10 hour exposure on a small part of this field taken using the 4.2 m William Herschel Telescope (WHT).

scholarly journals CCD Standard Fields

1993 ◽  
Vol 136 ◽  
pp. 73-78
Author(s):  
D.H.P. Jones
Keyword(s):  
Ccd Camera ◽  
Data Archive ◽  
Ccd Cameras ◽  
Isaac Newton ◽  
La Palma ◽  
Zero Points ◽  
Made In

AbstractThere are several standard fields for CCDs available in the literature. Some of these have been observed many times with the CCD cameras of the Isaac Newton Group of Telescopes on La Palma. These observations were made in order to establish the zero-points and colour equations for the U BV RI filters. Now that many observations are available in the data archive it is possible to combine them and search for inconsistencies in the published magnitudes and colours. This discussion will lead to standard fields of a higher quality. Furthermore astrometric plates have been taken of several of these fields which will be used to provide accurate positions as well as magnitudes and colours. These will provide the scale, orientation and distortion of any CCD camera.

scholarly journals Low Resolution Spectroscopy of 13 Low Surface Brightness PN's

1989 ◽  
Vol 131 ◽  
pp. 220-220
Author(s):  
A. Manchado ◽  
S. R. Pottasch ◽  
A. Mampaso
Keyword(s):  
Surface Brightness ◽  
Photon Counting ◽  
Outer Part ◽  
Low Resolution ◽  
Counting System ◽  
Isaac Newton ◽  
La Palma ◽  
Ionization Structure ◽  
Low Surface Brightness ◽  
Isaac Newton Telescope

We have obtained long-slit low resolution spectra (7.5 A resolution) of a sample of 13 low surface brightness planetary nebulae using the 2.5-m Isaac Newton Telescope (La Palma) with the Image Photon Counting System (IPCS) covering a spectral range from 3300 A to 7300 A. From those spectra we calculated the ionic and total abundances of 0, N, Ne and Ar. Variations in the ionization structure between the inner and the outer part are found in some nebulae although the total abundances appear not to change significantly along the nebulae.

scholarly journals Design of the 4.2m Herschel Telescope and Instruments

1982 ◽  
Vol 67 ◽  
pp. 49-59
Author(s):  
Paul Murdin
Keyword(s):  
Canary Islands ◽  
Research Council ◽  
Instrument Design ◽  
Royal Greenwich Observatory ◽  
Science And Engineering ◽  
Engineering Research ◽  
La Palma ◽  
The Uk ◽  
William Herschel

The UK Science and Engineering Research Council (SERC), through the Royal Greenwich Observatory (RGO), is installing on the island of La Palma, a 4.2 m altazimuth telescope, as part of the Observatorio del Roque de los Muchachos, at an altitude of 2300 m in the Canary Islands. The telescope, known as the William Herschel Telescope, is fully designed and manufacture has begun. It is due for completion in the mid-1980's. The telescope, dome and instrument design have all interacted with one another, particularly in the search for economy. Among the proposed instruments is a novel collimator-less spectrograph.

scholarly journals Co-ordinated Optical and Radio Observations of Symbiotic Stars

1990 ◽  
Vol 122 ◽  
pp. 442-443
Author(s):  
R. J. Ivison ◽  
M. F. Bode ◽  
J. Meaburn ◽  
R. J. Davis ◽  
R. F. Nelson ◽  
...  
Keyword(s):  
Broad Band ◽  
Symbiotic Stars ◽  
Echelle Spectrograph ◽  
Type Region ◽  
Isaac Newton ◽  
La Palma ◽  
Circumstellar Extinction ◽  
Optical Line ◽  
Isaac Newton Telescope ◽  
5 Ghz

AbstractWe present preliminary results from absolutely flux-calibrated optical spectroscopy, together with 5 GHz radio flux measures of 17 symbiotic stars. The data were obtained quasi-simultaneously using the Manchester Echelle Spectrograph on the Isaac Newton Telescope, La Palma between 1988 September 20 and 24, and the Broad Band Interferometer at Jodrell Bank during 1988 October. This represents the largest sample of these stars observed in this way to date. Distances are calculated using visual extinctions and are compared with other quoted values. In general, the agreement is surprisingly good. Plots of individual line luminosities vs. radio luminosity indicate that the D-type (dusty) symbiotics (both also proto-planetary nebulae) have far higher radio luminosities than S-types (stellar) for comparable recombination and forbidden line luminosities. This may however be due to underestimation of optical line luminosities for the D-types as the circumstellar extinction contribution is uncertain. The single D’-type (cool dust, yellow secondary) lies at the low luminosity end of the S-type region. ‘Very slow novae’ in our sample lie in both groups.

scholarly journals The visible and near-infrared spectra of asteroids in cometary orbits

2018 ◽  
Vol 618 ◽  
pp. A170 ◽  
Author(s):  
J. Licandro ◽  
M. Popescu ◽  
J. de León ◽  
D. Morate ◽  
O. Vaduvescu ◽  
...  
Keyword(s):  
Near Infrared ◽  
Spectral Slope ◽  
Isaac Newton ◽  
Infrared Telescope ◽  
La Palma ◽  
Spectral Class ◽  
Telescope Facility ◽  
Hydrated Minerals ◽  
Taxonomical Classification ◽  
William Herschel

Context. Dynamical and albedo properties suggest that asteroids in cometary orbits (ACOs) are dormant or extinct comets. Their study provides new insights for understanding the end-states of comets and the size of the comet population. Aims. We intend to study the visible and near-infrared (NIR) spectral properties of different ACO populations and compare them to the independently determined properties of comets. Methods. We select our ACOs sample based on published dynamical criteria and present our own observational results obtained using the 10.4 m Gran Telescopio Canarias (GTC), the 4.2 m William Herschel Telescope (WHT), the 3.56 m Telescopio Nazionale Galileo (TNG), and the 2.5 m Isaac Newton Telescope (INT), all located at the El Roque de los Muchachos Observatory (La Palma, Spain), and the 3.0 m NASA Infrared Telescope Facility (IRTF), located at the Mauna Kea Observatory, in Hawaii. We include in the analysis the spectra of ACOs obtained from the literature. We derive the spectral class and the visible and NIR spectral slopes. We also study the presence of hydrated minerals by studying the 0.7 μm band and the UV-drop below 0.5 μm associated with phyllosilicates. Results. We present new observations of 17 ACOs, 11 of them observed in the visible, 2 in the NIR and 4 in the visible and NIR. We also discuss the spectra of 12 ACOs obtained from the literature. All but two ACOs have a primitive-like class spectrum (X or D-type). Almost 100% of the ACOs in long-period cometary orbits (Damocloids) are D-types. Those in Jupiter family comet orbits (JFC-ACOs) are ∼60% D-types and ∼40% X-types. The mean spectral slope S′ of JFC-ACOs is 9.7 ± 4.6%/1000 Å and for the Damocloids this is 12.2 ± 2.0%/1000 Å. No evidence of hydration on the surface of ACOs is found from their visible spectra. The spectral slope and spectral class distribution of ACOs is similar to that of comets. Conclusions. The spectral taxonomical classification and the spectral slope distribution of ACOs, and the lack of spectral features indicative of the presence of hydrated minerals on their surface, strongly suggest that ACOs are likely dormant or extinct comets.

scholarly journals Multiband Photometry of NGC 7479 and NGC 7606

1996 ◽  
Vol 157 ◽  
pp. 123-125
Author(s):  
A. M. Varela ◽  
J. A. L. Aguerri ◽  
M. Prieto ◽  
C. Muñoz-Tuñón
Keyword(s):  
Spiral Galaxies ◽  
Three Dimensional ◽  
Surface Photometry ◽  
Dimensional Model ◽  
Three Dimensional Model ◽  
Isaac Newton ◽  
La Palma ◽  
Radial Profiles ◽  
Isaac Newton Telescope ◽  
Barred Spiral Galaxies

We present surface photometry in U BV RI passbands of the barred spiral galaxies NGC 7479 and NGC 7606, for which observations were obtained at the Cassegrain focus of the 2.5-m Isaac Newton Telescope at La Palma. Data are presented in the form of images and mean radial profiles from azimuthal fits of ellipses, giving the luminosity, ellipticities and position angles of the isophotes as functions of the galactocentric radii. Images in I-band are shown in Figure 1 of NGC 7479 (left) and NGC 7606 (right). These belong to a sample of galaxies with moderate circumnuclear starbursts. We are analyzing their structure to study the effects of departures from an axisymmetric potential for the dynamics of a galaxy. One objective of this study is to make a three-dimensional model of the bar and bulge using the method of photometric inversion. The sample consists of 27 spiral galaxies with and without a bar.

scholarly journals Optical validation and characterisation of Planck PSZ1 sources at the Canary Islands observatories

2020 ◽  
Vol 638 ◽  
pp. A146
Author(s):  
R. Barrena ◽  
A. Ferragamo ◽  
J. A. Rubiño-Martín ◽  
A. Streblyanska ◽  
A. Aguado-Barahona ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Gaussian Noise ◽  
Velocity Dispersion ◽  
Thermal Emission ◽  
Isaac Newton ◽  
La Palma ◽  
Second Year ◽  
Imaging And Spectroscopy ◽  
Non Gaussian ◽  
William Herschel

We report new galaxy clusters previously unknown included in the first Planck Sunyaev–Zeldovich (SZ) sources catalogue, the PSZ1. The results presented here were achieved during the second year of a two-year observational programme, the ITP13, developed at the Roque de los Muchachos Observatory (La Palma, Spain). Using the 2.5 m Isaac Newton telescope, the 3.5 m Telescopio Nazionale Galileo, the 4.2 m William Herschel telescope and the 10.4 m Gran Telescopio Canarias we characterised 75 SZ sources with low SZ significance, SZ S/N <  5.32. We performed deep optical imaging and spectroscopy in order to associate actual galaxy clusters with the SZ Planck source. We adopted robust criteria, based on the 2D spatial distribution, richness, and velocity dispersions to confirm actual optical counterparts up to z <  0.85. The selected systems are confirmed only if they are well aligned with respect to the PSZ1 coordinate and show high richness and high velocity dispersion. In addition, we also inspected the Compton y-maps and SZ significance in order to identify unrealistic detections. Following this procedure, we identify 26 cluster counterparts associated with the SZ emission, which means that only about 35% of the clusters considered in this low S/N PSZ1 subsample are validated. Forty-nine SZ sources (∼65% of this PSZ1 subset) remain unconfirmed. At the end of the ITP13 observational programme, we have studied 256 SZ sources with Dec ≥ −15° (212 of them completely unknown), finding optical counterparts for 152 SZ sources. The ITP13 validation programme has allowed us to update the PSZ1 purity, which is now more refined, increasing from 72% to 83% in the low SZ S/N regime. Our results are consistent with the predicted purity curve for the full PSZ1 catalogue and with the expected fraction of false detections caused by the non-Gaussian noise of foreground signals. We find a strong correlation between the number of unconfirmed sources and the thermal emission of diffuse galactic dust at 857 GHz, thus increasing the fraction of false Planck SZ detections at low galactic latitudes.

scholarly journals The Halos of NGC 6543 and NGC 6826

1989 ◽  
Vol 131 ◽  
pp. 196-196
Author(s):  
A. Manchado ◽  
S. R. Pottasch ◽  
A. Mampaso
Keyword(s):  
Photon Counting ◽  
Central Zone ◽  
Planetary Nebulae ◽  
Low Resolution ◽  
Electronic Temperature ◽  
Counting System ◽  
Isaac Newton ◽  
Physical Conditions ◽  
La Palma ◽  
Isaac Newton Telescope

Long slit low resolution (3.4 A) spectra of the planetary nebulae NGC 6543 and NGC 6826, obtained using the 2.5-m Isaac Newton Telescope (La Palma) with the Image Photon Counting System (IPCS), indicate different physical conditions in the outer halos than in the central zone, with an outward increase of electronic temperature. The estimated mass contained in these halos is considerably larger than the values of the inner nebulae.

scholarly journals Shock Modelling of the Bipolar Outflow Source NGC 6537

1993 ◽  
Vol 155 ◽  
pp. 385-385
Author(s):  
L. Cuesta ◽  
J. P. Phillips
Keyword(s):  
High Resolution ◽  
Narrow Band ◽  
Type I ◽  
High Excitation ◽  
Optical Telescope ◽  
Isaac Newton ◽  
Bipolar Outflow ◽  
La Palma ◽  
Large Shell ◽  
Isaac Newton Telescope

NGC 6537 is an unusual high excitation bipolar outflow source, with anomalous abundances indicative of a type I nebula. We have recently obtained a range of high resolution spectrophotometry for this source using the 2.5 m Isaac Newton Telescope (Observatorio del Roque de Los Muchachos, La Palma), together with narrow band optical imaging using the 2.6 m Nordic Optical Telescope (Observatorio del Roque de los Muchachos, La Palma). As a consequence, it is apparent that the source optical morphology is suggestive of the presence of an hyperbolic shock outflow surface, similar to those observed in other BPN (e.g. NGC 6302, Hb 5). Line ratio maps also indicate the presence of extremely strong [Nii] emission at the periphery of the outflow, whilst expansion velocities are of order ∼ 400 km sec−1. These large shell expansion velocities may in turn be driven by an extremely high velocity wind, which in this case appears to extend over a range ΔV ≥ 3000 km sec−1.

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