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 Andromeda galaxy (M31). As well as microlensing, the survey is sensitive to many different classes of variable stars and transients. In our first paper of this series, we reported the detection of 20 classical novae (CNe) observed in Sloan r' and i' passbands.

POINT-AGAPE pixel lensing survey of M31 - Evidence for a MACHO contribution to galactic halos

The POINT-AGAPE collaboration is carrying out a search for gravitational microlensing toward M31 to reveal galactic dark matter in the form of MACHOs (Massive Astrophysical Compact Halo Objects) in the halos of the Milky Way and M31. A high-threshold analysis of 3 years of data yields 6 bright, short- duration microlensing events, which are confronted to a simulation of the observations and the analysis. The observed signal is much larger than expected from self lensing alone and we conclude, at the 95% confidence level, that at least 20% of the halo mass in the direction of M31 must be in the form of MACHOs if their average mass lies in the range 0.5-1 M-circle dot. This lower bound drops to 8% for MACHOs with masses similar to 0.01 M-circle dot. In addition, we discuss a likely binary microlensing candidate with caustic crossing. Its location, some 32' away from the centre of M31, supports our conclusion that we are detecting a MACHO signal in the direction of M31.

The POINT-AGAPE survey - II. An unrestricted search for microlensing events towards M31

An automated search is carried out for microlensing events using a catalogue of 44 554 variable superpixel light curves derived from our 3-yr monitoring programme of M31. Each step of our candidate selection is objective and reproducible by a computer. Our search is unrestricted, in the sense that it has no explicit time-scale cut. So, it must overcome the awkward problem of distinguishing long time-scale microlensing events from long-period stellar variables.

Classical novae from the POINT-AGAPE microlensing survey of M31 - I. The nova catalogue

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 Andromeda galaxy (M31). As well as microlensing, the survey is sensitive to many different classes of variable stars and transients. Here we describe the automated detection and selection pipeline used to identify M31 classical novae (CNe) and we present the resulting catalogue of 20 CN candidates observed over three seasons. CNe are observed both in the bulge region as well as over a wide area of the M31 disc. Nine of the CNe are caught during the final rise phase and all are well sampled in at least two colours. The excellent light-curve coverage has allowed us to detect and classify CNe over a wide range of speed class, from very fast to very slow. Among the light curves is a moderately fast CN exhibiting entry into a deep transition minimum, followed by its final decline. We have also observed in detail a very slow CN which faded by only 0.01 mag d(-1) over a 150-d period. We detect other interesting variable objects, including one of the longest period and most luminous Mira variables. The CN catalogue constitutes a uniquely well-sampled and objectively-selected data set with which to study the statistical properties of CNe in M31, such as the global nova rate, the reliability of novae as standard-candle distance indicators and the dependence of the nova population on stellar environment. The findings of this statistical study will be reported in a follow-up paper.

The POINT-AGAPE survey - I. The variable stars in M31

For the purposes of identifying microlensing events, the POINT-AGAPE collaboration has been monitoring the Andromeda galaxy (M31) for three seasons (1999-2001) with the Wide Field Camera on the Isaac Newton Telescope. In each season, data are taken for one hour per night for roughly 60 nights during the six months that M31 is visible. The two 33 x 33 arcmin(2) fields of view straddle the central bulge, northwards and southwards. We have calculated the locations, periods and brightness of 35 414 variable stars in M31 as a by-product of the microlensing search. The variables are classified according to their period and brightness. Rough correspondences with classical types of variable star (such as Population I and II Cepheids, Miras and semiregular long-period variables) are established. The spatial distribution of Population I Cepheids is clearly associated with the spiral arms, while the central concentration of the Miras and long-period variables varies noticeably, the brighter and the shorter period Miras being much more centrally concentrated.

The POINT-AGAPE survey: 4 high signal-to-noise microlensing candidates detected towards M 31

We have carried out a survey of the Andromeda galaxy for unresolved microlensing (pixel lensing). We present a subset of four short timescale, high signal-to-noise microlensing candidates found by imposing severe selection criteria: the source flux variation exceeds the flux of an R = 21 magnitude star and the full width at half maximum timescale is less than 25 days. Remarkably, in three out of four cases, we have been able to measure or strongly constrain the Einstein crossing time of the event. One event, which lies projected on the M 31 bulge, is almost certainly due to a stellar lens in the bulge of M 31. The other three candidates can be explained either by stars in M 31 and M 32 or by MACHOs.

A short-timescale candidate microlensing event in the point-agape pixel lensing survey of M31

We report the discovery of a short-duration microlensing candidate in the northern field of the POINT-AGAPE pixel lensing survey toward M31. Almost certainly, the source star has been identified on Hubble Space Telescope archival images, allowing us to infer an Einstein crossing time of t(E) = 10.4 days, a maximum magnification of A(max) similar to 18, and a lens-source proper motion mu (rel) > 0.3 mu as day(-1). The event has a projected separation of 8' from the center of M31, beyond the bulk of the stellar lens population. There are three plausible identifications/locations for the lensing object: a massive compact halo object (MACHO) in either M31 or the Milky Way, or a star in the M31 disk. The most probable mass is 0.06 M-. for an M31 MACHO, 0.02 M-. for a Milky Way MACHO, and 0.2 M-. for an M31 stellar lens. While the stellar interpretation is possible, the MACHO interpretation is the most probable for halo fractions above 20%.

Agape??smo y eros pedag??gico en el sistema preventivo de Don Bosco

Resumen basado en el de la publicaci??n

Die Agape; oder, Der geheime weltbund der Christen, von Klemens in Rom unter Domitians regierung gestiftet;

Added t.-p.: Versuch einer schilderung der Agape in ihrem ersten jahrhunderte.

Marcelian charm in nursing practice: The unity of agape and eros as the foundation of an ethic of care

Abstract In the nursing literature, a number of qualities are associated with loving care. Reference is made to, among other things, humility, attentiveness, responsibility and duty, compassion, and tenderness. The author attempts to show that charm, in the Marcelian sense, also plays a central role. It is argued that the moral foundation of charm is a unity of agape and eros. An impartial giving of the self for others is clearly of fundamental importance in an ethic of care. Including charm in the discussion points to the fact that eros also plays a crucial role. Eros produces a passion for people and for life. It is a physical and spiritual energy that animates a person in all facets of her life, including her caring work.

Dialogisuus ja kohtaaminen : Tutkimus kristillisten koulujen toimintakulttuurista kasvatussuhteen näkökulmasta

The main focus of this research was to describe the educational purpose of Christian schools within their operation culture. The Christian schools founded in Finland can be seen as part of a greater movement in Europe. In this research the dialogue and encounter in the educational scheme of Finnish Christian schools were examined by asking three research questions: 1. What is the nature of the dialogue in education in Finnish Christian schools? 2. How do the teachers describe themselves as educators? 3. What are the special characteristics in the operation culture of a Christian school? The educational relationship was regarded as fundamental and in the background reflected the absolute value of each student. Communication skills were viewed as essential in the building of relationships, which also included emotion communication skills as a broader view. The teachers expressed their comprehension of the meaning of the dialogue in the building of a relationship with practical examples. Students learned to understand one another's experiences by discussion and listening to one another. The values that created a connection were mutual appreciation, honesty, taking the other one into account, and the ability for empathy. Caring was regarded as a relationship between people, as well as a genuine mutual encounter, in which all parties would listen to one another and be heard by others. The respondents thought that individual attention and time were the keys to reaching well-being and an encounter. Students' commitment to the community was supported by mutual agreements, identifying with the common world, and encounters. The appearance of Christian love agape was named as the basis for an educational relationship. The answers emphasised shared everyday life at school. According to the teachers, the willingness for personal growth enabled encounters, although growth as such was often regarded as difficult. Cognitive emphasising and emotional experiencing from a dynamic perspective, were the means by which students' ethical understanding was comprehended. The teachers named three key factors to create a confidential relationship: a respectful attitude, courage, and genuineness. Within the school operational environment, a sense of community was emphasised, in which each student was taken into account individually. The active role of parents was an essential part of the school culture. The administration of the schools appeared committed. The additional pressure in school work came from efforts to ensure the official status of the school, as well as the large amount of administrative work involved in a private school. According to the research data, there was no evidence to support any elitism that is often associated with private schools.

Kantin käsitys ystävyydestä ja rakkaudesta

Tässä tutkielmassa tarkastellaan Immanuel Kantin käsitystä ideaalista ystävyydestä. Tarkoituksena oli ratkaista sen olemassa olo rakkauden vastavuoroisuuden perusteella. Ystävyys on ollut antiikista lähtien filosofialle merkittävä ongelma. Immanuel Kant käsittelee ystävyyttä kahdessa teoksessaan The Metaphysics of Morals ja Lectures on Ethics. Kantin ystävyyskäsitys sisältää neljä erilaista ystävyyden lajia. Ne ovat tarveystävyys, esteettinen ystävyys, intiimiystävyys ja ideaali ystävyys. Tarveystävyys perustuu hyödyn tavoittelulle. Esteettisellä ystävyydellä tarkoitetaan nautintoja hakevaa ystävyyttä. Intiimiystävyys on luonteen ystävyyttä. Ideaali ystävyys on Kantin käsitys täydellisestä ystävyydestä. Ideaalissa ystävyydessä niin kuin intiimiystävyydessä tärkeintä on keskusteleminen. Rakkauden tasapainon selvittämiseksi tutustuttiin Kantin käsityksiin rakkaudesta. Rakkauden lajeja Kantilta esittelin viisi. Niiden lisäksi onnellisuus oli tunne, joka vaikutti ystävyyden muodostumiseen. Rakkauden lajeja ovat itserakkaus, eros, agape, philia ja amor benevolentiae. Itserakkaus on itsensä rakastamista. Eros on intohimoa korostava rakkauden laji. Se kuuluu avioliittoon, ei ystävyyteen. Agape tunnetaan lähimmäisenrakkautena. Philia eroaa agapesta siten, että se on kiinnostunut joistain rakastettavista piirteistä toisessa yksilössä. Amor benevolentiae on hyväntahtoisuuden osoittamista. Rakkaus, joka ystävien välillä ilmeni vastavuoroisena, vahvistui lajiltaan philiaksi. Vastavuoroisuus ystävien kesken vaatii ajan ja paikan. Vastavuoroisuutta vaikeuttaa epävarmuus siitä. Vastavuoroisuudesta on saatava runsaasti todisteita. Todisteita saadaan tavoilla, jotka ystävät ymmärtävät. Ymmärtäminen edellyttää yhteisiä viestintäkeinoja. Kun tarpeeksi toisiinsa luottavat ystävät keskustelevat keskenään, he myös muovaavat toistensa persoonia. Silloin he tekevät toisistaan rakastettavampia. Tutkimukseni perusteella ideaali ystävyys on mahdollinen. Vastavuoroisuus rakkaudessa onnistuu, jos ystävät muokkaavat toisiaan. Ideaali ystävyys on molemminpuolisen kehittymisen tulos, jolloin ystävät tekevät toisistaan itsensä kaltaisia ja pystyvät rakastamaan toista kuin itseään.

Kantin käsitys ystävyydestä ja rakkaudesta

Tässä tutkielmassa tarkastellaan Immanuel Kantin käsitystä ideaalista ystävyydestä. Tarkoituksena oli ratkaista sen olemassa olo rakkauden vastavuoroisuuden perusteella. Ystävyys on ollut antiikista lähtien filosofialle merkittävä ongelma. Immanuel Kant käsittelee ystävyyttä kahdessa teoksessaan The Metaphysics of Morals ja Lectures on Ethics. Kantin ystävyyskäsitys sisältää neljä erilaista ystävyyden lajia. Ne ovat tarveystävyys, esteettinen ystävyys, intiimiystävyys ja ideaali ystävyys. Tarveystävyys perustuu hyödyn tavoittelulle. Esteettisellä ystävyydellä tarkoitetaan nautintoja hakevaa ystävyyttä. Intiimiystävyys on luonteen ystävyyttä. Ideaali ystävyys on Kantin käsitys täydellisestä ystävyydestä. Ideaalissa ystävyydessä niin kuin intiimiystävyydessä tärkeintä on keskusteleminen. Rakkauden tasapainon selvittämiseksi tutustuttiin Kantin käsityksiin rakkaudesta. Rakkauden lajeja Kantilta esittelin viisi. Niiden lisäksi onnellisuus oli tunne, joka vaikutti ystävyyden muodostumiseen. Rakkauden lajeja ovat itserakkaus, eros, agape, philia ja amor benevolentiae. Itserakkaus on itsensä rakastamista. Eros on intohimoa korostava rakkauden laji. Se kuuluu avioliittoon, ei ystävyyteen. Agape tunnetaan lähimmäisenrakkautena. Philia eroaa agapesta siten, että se on kiinnostunut joistain rakastettavista piirteistä toisessa yksilössä. Amor benevolentiae on hyväntahtoisuuden osoittamista. Rakkaus, joka ystävien välillä ilmeni vastavuoroisena, vahvistui lajiltaan philiaksi. Vastavuoroisuus ystävien kesken vaatii ajan ja paikan. Vastavuoroisuutta vaikeuttaa epävarmuus siitä. Vastavuoroisuudesta on saatava runsaasti todisteita. Todisteita saadaan tavoilla, jotka ystävät ymmärtävät. Ymmärtäminen edellyttää yhteisiä viestintäkeinoja. Kun tarpeeksi toisiinsa luottavat ystävät keskustelevat keskenään, he myös muovaavat toistensa persoonia. Silloin he tekevät toisistaan rakastettavampia. Tutkimukseni perusteella ideaali ystävyys on mahdollinen. Vastavuoroisuus rakkaudessa onnistuu, jos ystävät muokkaavat toisiaan. Ideaali ystävyys on molemminpuolisen kehittymisen tulos, jolloin ystävät tekevät toisistaan itsensä kaltaisia ja pystyvät rakastamaan toista kuin itseään.

Theory of pixel lensing toward M31. II. The velocity anisotropy and flattening of the MACHO distribution

The POINT-AGAPE collaboration is currently searching for massive compact halo objects (MACHOs) toward the Andromeda galaxy (M31). The survey aims to exploit the high inclination of the M31 disk, which causes an asymmetry in the spatial distribution of M31 MACHOs. Here, we investigate the effects of halo velocity anisotropy and flattening on the asymmetry signal using simple halo models. For a spherically symmetric and isotropic halo, we find that the underlying pixel lensing rate in far-disk M31 MACHOs is more than 5 times the rate of near-disk events. We find that the asymmetry is further increased by about 30% if the MACHOs occupy radial orbits rather than tangential orbits, but it is substantially reduced if the MACHOs lie in a flattened halo. However, even for halos with a minor- to major-axis ratio of q = 0.3, the number of M31 MACHOs in the far side outnumber those in the near side by a factor of similar to2. There is also a distance asymmetry, in that the events on the far side are typically farther from the major axis. We show that, if this positional information is exploited in addition to number counts, then the number of candidate events required to confirm asymmetry for a range of flattened and anisotropic halo models is achievable, even with significant contamination by variable stars and foreground microlensing events. For pixel lensing surveys that probe a representative portion of the M31 disk, a sample of around 50 candidates is likely to be sufficient to detect asymmetry within spherical halos, even if half the sample is contaminated, or to detect asymmetry in halos as flat as q = 0.3, provided less than a third of the sample comprises contaminants. We also argue that, provided its mass-to-light ratio is less than 100, the recently observed stellar stream around M31 is not problematic for the detection of asymmetry.

Theory of pixel lensing towards M31 - I. The density contribution and mass of MACHOs

POINT-AGAPE is an Angle-French collaboration which is employing the Isaac Newton Telescope (INT) to conduct a pixel-lensing survey towards M31. Pixel lensing is a technique which permits the detection of microlensing against unresolved stellar fields. The survey aims to constrain the stellar population in M31, and also the distribution and nature of massive compact halo objects (MACHOs) in both M31 and the Galaxy.