OGLE Atlas of Classical Novae I. Galactic Bulge Objects

  title={OGLE Atlas of Classical Novae I. Galactic Bulge Objects},
  author={Przemek Mr{\'o}z and Andrzej Udalski and Radosław Poleski and Igor Soszyński and Michał K. Szymański and Grzegorz Pietrzyński and Lukasz Wyrzykowski and Krzysztof Ulaczyk and Szymon Kozłowski and Paweł Pietrukowicz and Jan Skowron},
  journal={Astrophysical Journal Supplement Series},
Eruptions of classical novae are possible sources of lithium formation and gamma-ray emission. Nova remnants can also become Type Ia supernovae (SNe Ia). The contribution of novae to these phenomena depends on nova rates, which are not well established for the Galaxy. Here, we directly measure a Galactic bulge nova rate of $13.8 \pm 2.6$ per year. This measurement is much more accurate than any previous measurement of this kind thanks to many years' monitoring of the bulge by the Optical… 
OGLE Atlas of Classical Novae. II. Magellanic Clouds
The population of classical novae in the Magellanic Clouds was poorly known because of a lack of systematic studies. There were some suggestions that nova rates per unit mass in the Magellanic Clouds
Observations of galactic and extragalactic novae
The recent GAIA DR2 measurements of distances to galactic novae have allowed to re-analyse some properties of nova populations in the Milky Way and in external galaxies on new and more solid
V5852 Sgr: an unusual nova possibly associated with the Sagittarius stream
We report spectroscopic and photometric follow-up of the peculiar nova V5852~Sgr (discovered as OGLE-2015-NOVA-01), which exhibits a combination of features from different nova classes. The
A Population of Heavily Reddened, Optically Missed Novae from Palomar Gattini-IR: Constraints on the Galactic Nova Rate
The nova rate in the Milky Way remains largely uncertain, despite its vital importance in constraining models of Galactic chemical evolution as well as understanding progenitor channels for Type Ia
Galactic Extinction: How Many Novae Does It Hide and How Does It Affect the Galactic Nova Rate?
There is a long-standing discrepancy between the observed Galactic classical nova rate of ∼10 yr−1 and the predicted rate from Galactic models of ∼30–50 yr−1. One explanation for this discrepancy is
Shock-powered radio emission from V5589 Sagittarii (Nova Sgr 2012 #1)
Since the Fermi discovery of $\gamma$-rays from novae, one of the biggest questions in the field has been how novae generate such high-energy emission. Shocks must be a fundamental ingredient. Six
Despite its fundamental importance, a reliable estimate of the Galactic nova rate has remained elusive. Here, the overall Galactic nova rate is estimated by extrapolating the observed rate for novae
A Hubble Space Telescope Survey for Novae in M87. I. Light and Color Curves, Spatial Distributions and the Nova Rate
The Hubble Space Telescope has imaged the central part of M87 over a 10 week span, leading to the discovery of 32 classical novae and nine fainter, likely very slow and/or symbiotic novae. In this
Search for gamma-ray emission from Galactic novae with the Fermi -LAT
Context. A number of novae have been found to emit high-energy gamma rays (>100 MeV). However, the origin of this emission is not yet understood. We report on the search for gamma-ray emission from
Nucleosynthesis constraints through γ-ray line measurements from classical novae
Context. Classical novae belong to the most frequent transient events in the Milky Way and are key agents of ongoing nucleosynthesis. Despite their large numbers, they have never been observed in


Recurrent and symbiotic novae in data from the Optical Gravitational Lensing Experiment
We analyse long-term optical photometry for two Galactic recurrent novae (V745 Sco and V3890 Sgr) and one Large Magellanic Cloud object (Nova LMC 1990b) observed over several years by the Optical
A pr 2 00 7 XMM-Newton observations of Nova Sgr 1998
We report on X-ray observations of Nova Sagittarius 1998 (V4633 Sgr), performed with XMM-Newton at three different epochs, 934, 1083 and 1265 days after discovery. The nova was detected with the EPIC
Classical novae from the POINT-AGAPE microlensing survey of M31 - II. Rate and statistical characteristics of the nova population
The POINT-AGAPE (Pixel-lensing Observations with the Isaac Newton Telescope- Andromeda Galaxy Amplified Pixels Experiment) survey is an optical search for gravitational microlensing events towards
The nova rate in the elliptical component of NGC 5128
The results are presented of a five year nova survey of NGC 5128 performed with an H-alpha filter at the prime focus of the CTIO 4 m telescope. In all, 16 novae were detected, of which 12 are members
An accreting white dwarf near the Chandrasekhar limit in the andromeda galaxy
The intermediate Palomar Transient Factory (iPTF) detection of the most recent outburst of the recurrent nova (RN) system RX J0045.4+4154 in the Andromeda galaxy has enabled the unprecedented study
Identification of V1017 Sgr as a cataclysmic variable binary system with unusually long period
CLASSICAL and dwarf novae are both binary star systems in which mass is transferred onto a white-dwarf primary from a red-dwarf secondary that overflows its Roche lobe. In classical novae, mass
The hunt for old novae
We inform on the progress of our on-going project to identify and classify old classical novae, using deep UBVR photometry and subsequent spectroscopy for a proper candidate confirmation, and
V5116 Sagittarii, an Eclipsing Supersoft Postoutburst Nova?
V5116 Sgr (Nova Sgr 2005 No. 2), discovered on 2005 July 4, was observed with XMM-Newton in 2007 March, 20 months after the optical outburst. The X-ray spectrum shows that the nova had evolved to a
Life after eruption – II. The eclipsing old nova V728 Scorpii
The old nova V728 Sco has been recently recovered via photometric and spectroscopic observations, 150 yr after the nova eruption. The spectral properties pointed to a high-inclination system with a
A Universal Decline Law of Classical Novae
We calculate many different nova light curves for a variety of white dwarf masses and chemical compositions, with the assumption that free-free emission from optically thin ejecta dominates the