Islandscapes and ‘Islandness’: The Prehistoric Isle of Man in the Irish Seascape

Frieman, Catherine J.

doi:10.1111/j.1468-0092.2008.00301.x

Cited by 39 publications

(41 citation statements)

References 27 publications

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“…We chose to announce most of the obvious SNe with bright hosts in CBETs and these were usually spectroscopically followed and thus confirmed. Although significant follow-up would be required to characterize all the OTs discovered by CRTS, this is possible as the SDSS-II Supernova Survey acquired ∼180 nights of spectroscopic time on 2.4-11 m telescopes, to follow SNe found during ∼70 nights of imaging (Frieman et al 2008). All OTs will continue to be made publicly available from VOEventNet and those events that appear the most interesting will be announced in ATels and CBETs.…”

Section: Summary and Discussionmentioning

confidence: 99%

First Results From the Catalina Real-Time Transient Survey

Drake¹,

Djorgovski²,

Mahabal³

et al. 2009

ApJ

1,293

1,131

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We report on the results from the first six months of the Catalina Real-Time Transient Survey (CRTS). In order to search for optical transients (OTs) with timescales of minutes to years, the CRTS analyses data from the Catalina Sky Survey which repeatedly covers 26,000 of square degrees on the sky. The CRTS provides a public stream of transients that are bright enough to be followed up using small telescopes. Since the beginning of the survey, all CRTS transients have been made available to astronomers around the world in real time using HTML tables,RSS feeds, and VOEvents. As part of our public outreach program, the detections are now also available in Keyhole Markup Language through Google Sky. The initial discoveries include over 350 unique OTs rising more than 2 mag from past measurements. Sixty two of these are classified as supernovae (SNe), based on light curves, prior deep imaging and spectroscopic data. Seventy seven are due to cataclysmic variables (CVs; only 13 previously known), while an additional 100 transients were too infrequently sampled to distinguish between faint CVs and SNe. The remaining OTs include active galactic nucleus, blazars, high-proper-motions stars, highly variable stars (such as UV Ceti stars), and transients of an unknown nature. Our results suggest that there is a large population of SNe missed by many current SN surveys because of selection biases. These objects appear to be associated with faint host galaxies. We also discuss the unexpected discovery of white dwarf binary systems through dramatic eclipses.

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Section: Summary and Discussionmentioning

confidence: 99%

First Results From the Catalina Real-Time Transient Survey

Drake¹,

Djorgovski²,

Mahabal³

et al. 2009

ApJ

1,293

1,131

View full text Add to dashboard Cite

show abstract

“…The quality of the 303 runs changes from optimal seeing, sky brightness and photometric conditions for 84 runs obtained between 1998 and 2004 to 219 additional runs where the conditions were poorer including worst seeing, bright moonlight and/or non-photometric skies. These last runs were obtained from 2005 to 2007 as part of the SDSS-II Supernovae Survey (Frieman et al 2008).…”

Section: Datamentioning

confidence: 99%

The IAC Stripe 82 Legacy Project: a wide-area survey for faint surface brightness astronomy

Fliri¹,

Trujillo²

2015

Mon. Not. R. Astron. Soc.

135

118

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We present new deep co-adds of data taken within Stripe 82 of the Sloan Digital Sky Survey (SDSS), especially stacked to reach the faintest surface brightness limits of this data set. Stripe 82 covers 275 deg 2 within -50 • RA +60 • and -1.• 25 Dec. +1.• 25. We discuss the steps of our reduction which puts special emphasis on preserving the characteristics of the background (sky + diffuse light) in the input images using a non-aggressive sky subtraction strategy. Our reduction reaches a limit of ∼28.5 mag arcsec −2 (3σ, 10×10 arcsec 2 ) in the r band. The effective surface brightness limit (50% completeness for exponential light distribution) lies at < µ e (r) >∼25.5 mag arcsec −2 . For point sources, we reach 50% completeness limits (3σ level) of (24.2, 25.2, 24.7, 24.3, 23.0) mag in (u, g, r, i, z). This is between 1.7 and 2.0 mag deeper than the single-epoch SDSS releases. The co-adds show point spread functions (PSFs) with median full width at half-maximum values ranging from 1 arcsec in i and z to 1.3 arcsec in the u band. The imaging data are made publicly available at http://www.iac.es/proyecto/stripe82. The release includes deep co-adds and representations of the PSF for each field. Additionally, we provide object catalogues with stars and galaxies confidently separated until g∼23 mag. The IAC Stripe 82 co-adds offer a rather unique possibility to study the low surface brightness Universe, exemplified by the discovery of stellar streams around NGC0426 and NGC0936. We also discuss further science cases like stellar haloes and disc truncations, low surface brightness galaxies, the intra-cluster light in galaxy clusters and the diffuse emission of Galactic dust known as Galactic Cirrus.

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“…The Type Ia template in this fitting is constructed by Hsiao et al (2007) and Type II templates are condtructed by 12 observed Type II SNe (e.g. SDSS-II SN survey / Frieman et al 2008). After this stage, 50 variable objects remain as SN Ia candidates.…”

Section: Rate Calculationmentioning

confidence: 99%

A rate study of Type Ia supernovae with Subaru/XMM-Newton Deep Survey

Ihara¹,

Doi²,

Morokuma³

et al. 2009

Proc. IAU

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Abstract. We present a measurement of the rate of high-z Type Ia supernovae (SNe Ia) using multi-epoch observations of Subaru/XMM-Newton Deep Field (SXDF) with Suprime-Cam on the Subaru Telescope. Although SNe Ia are regarded as a standard candle, progenitor systems of SNe Ia have not been resolved yet. One of the key parameters to show the progenitor systems by observations is the delay time distribution between the binary system formation and subsequent SN explosion. Recently, a wide range of delay time is studied by SN Ia rates compared with an assumed cosmic star formation history. If SNe Ia with short delay time are dominant, the cosmic SN Ia rate evolution should closely trace that of the cosmic star formation. In order to detect a lot of high-z SNe Ia and measure SN Ia rates, we repeatedly carried out wide and deep imaging observations in the i -band with Suprime-Cam in 2002 (FoV∼1 deg 2 , mi < 25.5 mag). We obtained detailed light curves of the variable objects, and 50 objects are classified as SNe Ia using the light curve fitting method at the redshift range of 0.2 < z < 1.3. In order to check the completeness and contamination of the light curve classification method, we performed Monte Carlo simulations and generated ∼100,000 light curves of SNe Ia and II from templates. The control time and detection efficiency of the SN survey are also calculated using the artificial light curves. We derived an increasing trend of rates at around z ∼ 1.2. Our results are almost consistent with other SN Ia rate results from low-z to high-z. Our results are the first results of high-z SN Ia rates with large statistics using light curves obtained by ground based telescopes, and give us visions of the SN rate studies for the future. MotivationStudying the rate of Type Ia supernovae (SNe Ia) is very important to understand the progenitor of SNe Ia. The dependence of SN Ia rates on properties of host galaxies indicates a wide range of the delay time between the binary system formation and subsequent SN explosion, from 1Gyr to ∼10 Gyr (Mannucci et al. 2006). Recently, a more quantitative measurement of the delay time distribution (DTD) of SNe Ia has been made by Totani et al. (2008), and DTD is well described as ∝ t −1 in 0.1-10 Gyr, confirming that DTD extends to short delay time of 0.1 Gyr. Because of the existence of short delay time SNe Ia, it is predicted that the cosmic SN Ia rate evolution should closely trace that of the cosmic star formation, and hence SN Ia rates should be increasing with redshift toward the peak of the cosmic SFR at z ∼ 2 − 3 (e.g., Hopkins & Beacon 2006). Measuring high-z (z > 1.0) SN Ia rates is very difficult because SNe Ia are too faint (m i > 25 mag), and we need 8-m class telescopes or the Hubble Space Telescope (HST). Dahlen et al. (2008) (here after D08) reported the highest-z SN Ia rates with HST. Interestingly, their SN Ia rates show a decrease beyond z ∼ 1.6, which is in contradiction with the expectation from the DTD measurements. However, the D08 rates have large 358 available at ht...

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Islandscapes and ‘Islandness’: The Prehistoric Isle of Man in the Irish Seascape

Abstract: 1However, Davey and Innes (2002, 53-54) have rather unconvincingly made a preliminary argument for periods of abandonment followed by new colonization throughout Manx earlier prehistory.

Cited by 39 publications

References 27 publications

First Results From the Catalina Real-Time Transient Survey

First Results From the Catalina Real-Time Transient Survey

The IAC Stripe 82 Legacy Project: a wide-area survey for faint surface brightness astronomy

A rate study of Type Ia supernovae with Subaru/XMM-Newton Deep Survey

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