Search

Your search keyword '"Kalfountzou, E."' showing total 23 results
Start Over Author "Kalfountzou, E."
23 results on '"Kalfountzou, E."'

1. CIELO-RGS: a catalogue of soft X-ray ionized emission lines

Author

Mao, Junjie, Kaastra, J. S., Guainazzi, M., Gonzalez-Riestra, R., Santos-LLeo, M., Kretschmar, P., Grinberg, V., Kalfountzou, E., Ibarra, A., Matzeu, G., Parker, M., and Rodriguez-Pascual, P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

High-resolution X-ray spectroscopy has advanced our understanding of the hot Universe by revealing physical properties like kinematics, temperature, and abundances of the astrophysical plasmas. Despite the technical and scientific achievements, the lack of scientific products at a level higher than count spectra is hampering full scientific exploitation of high-quality data. This paper introduces the Catalogue of Ionized Emission Lines Observed by the Reflection Grating Spectrometer (CIELO-RGS) onboard the XMM-Newton space observatory. The CIELO-RGS catalogue aims to facilitate the exploitation of emission features in the public RGS spectra archive, in particular, to perform the correlation between X-ray spectral diagnostics parameters with measurements at other wavelengths. This paper focuses on the methodology of catalogue generation, describing the automated line detection algorithm. A moderate sample (~2400 observations) of high-quality RGS spectra available at XMM-Newton Science Archive is used as our starting point. A list of potential emission lines is selected based on a multi-scale peak detection algorithm in a uniform and automated way without prior assumption on the underlying astrophysical model. The candidate line list is validated via spectral fitting with simple continuum and line profile models. We also compare the catalogue content with published literature results on a small number of exemplary sources. We generate a catalogue of emission lines ~12000 detected in ~1600 observations toward stars, X-ray binaries, supernovae remnants, active galactic nuclei, and groups and clusters of galaxies. For each line, we report the observed wavelength, broadening, energy and photon flux, and equivalent width, etc., Comment: accepted to A&A

Published
2019
Full Text
View/download PDF

2. A high velocity component to the complex absorption in IRAS 13349+2438

Author

Parker, M. L., Matzeu, G. A., Guainazzi, M., Kalfountzou, E., Miniutti, G., Santos-Lleó, M., and Schartel, N.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present an analysis of XMM-Newton spectra of the low-redshift quasar IRAS 13349+2438. The RGS spectrum shows a large number of absorption lines from two zones of warm absorption, with velocities of $\sim$-600 km s$^{-1}$, as noted by previous authors. Additionally, we find robust evidence from multiple Ly{\alpha} absorption lines for a previously undiscovered ultra-fast zone of absorption, with an outflow velocity of $-0.13\pm0.01c$. The warm absorbers and ultra-fast outflow have similar mass outflow rates, around 40% of the Eddington accretion rate, but the kinetic power is dominated by the high velocity gas, which has a power of $\sim$4% of the Eddington luminosity., Comment: 13 pages, 13 figures, accepted for publication in MNRAS

Published
2018
Full Text
View/download PDF

3. Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Author

Kalfountzou, E., Stevens, J. A., Jarvis, M. J., Hardcastle, M. J., Wilner, D., Elvis, M., Page, M. J., Trichas, M., and Smith, D. J. B.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Several studies support the existence of a link between the AGN and star formation activity. Radio jets have been argued to be an ideal mechanism for direct interaction between the AGN and the host galaxy. A drawback of previous surveys of AGN is that they are fundamentally limited by the degeneracy between redshift and luminosity in flux-density limited samples. To overcome this limitation, we present far-infrared Herschel observations of 74 radio-loud quasars (RLQs), 72 radio-quiet quasars (RQQs) and 27 radio galaxies (RGs), selected at 0.9

Published
2017
Full Text
View/download PDF

4. The XXL survey: first results and future

Author

Pierre, M., Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Brun, A. Le, Maughan, B., Maurogordato, S., McCarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferrari, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Fevre, J. -P. Le, Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., McGee, S., Melin, J. -B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Ranalli, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, M., Sauvageot, J. -L., Schimd, C., Sereno, M., Smith, G. P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., and Truong, N.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The XXL survey currently covers two 25 sq. deg. patches with XMM observations of ~10ks. We summarise the scientific results associated with the first release of the XXL data set, that occurred mid 2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z<2) cluster, (z<4) AGN and cosmic background survey science will then benefit from an extraordinary data reservoir. This, combined with deep multi-$\lambda$ observations, will lead to solid standalone cosmological constraints and provide a wealth of information on the formation and evolution of AGN, clusters and the X-ray background. In particular, it will offer a unique opportunity to pinpoint the z>1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions., Comment: Proceeding of the XMM Next Decade Workshop held at ESAC, 9-11 May 2016

Published
2016
Full Text
View/download PDF

5. The Largest X-ray Selected Sample of z>3 AGNs: C-COSMOS & ChaMP

Author

Kalfountzou, E., Civano, F., Elvis, M., Trichas, M., and Green, P.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present results from an analysis of the largest high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) sample to date, combining the Chandra C-COSMOS and ChaMP surveys and doubling the previous samples. The sample comprises 209 X-ray-detected AGN, over a wide range of rest frame 2-10 keV luminosities logL_{X}=43.3 - 46.0 erg s^{-1}. X-ray hardness rates show that ~39% of the sources are highly obscured, N_{H}>10^{22} cm^{-2}, in agreement with the ~37% of type-2 AGN found in our sample based on their optical classification. For ~26% of objects have mismatched optical and X-ray classifications. Using the 1/V_{max} method, we confirm that the comoving space density of all luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~ 7. With a significant sample of AGN (N=27) at z > 4, it is found that both source number counts in the 0.5 -2 keV band and comoving space density are consistent with the expectation of a luminosity dependent density evolution (LDDE) model at all redshifts, while they exclude the luminosity and density evolution (LADE) model. The measured comoving space density of type-1 and type-2 AGN shows a constant ratio between the two types at z > 3. Our results for both AGN types at these redshifts are consistent with the expectations of LDDE model., Comment: 20 pages, 11 figures. Accepted to MNRAS

Published
2014
Full Text
View/download PDF

6. Herschel-ATLAS: Far-infrared properties of radio-loud and radio-quiet quasars

Author

Kalfountzou, E., Stevens, J. A., Jarvis, M. J., Hardcastle, M. J., Smith, D. J. B., Bourne, N., Dunne, L., Ibar, E., Eales, S., Ivison, R. J., Maddox, S., Smith, M. W. L., Valiante, E., and de Zotti, G.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have constructed a sample of radio-loud and radio-quiet quasars from the Faint Im- ages Radio Sky at Twenty-one centimetres (FIRST) and the Sloan Digital Sky Survey Data Release 7 (SDSS DR7), over the H-ATLAS Phase 1 Area (9h, 12h and 14.5h). Using a stacking analysis we find a significant correlation between the far-infrared luminosity and 1.4-GHz luminosity for radio-loud quasars. Partial correlation analysis confirms the intrinsic correlation after removing the redshift contribution while for radio-quiet quasars no partial correlation is found. Using a single-temperature grey-body model we find a general trend of lower dust temperatures in the case of radio-loud quasars comparing to radio-quiet quasars. Also, radio-loud quasars are found to have almost constant mean values of dust mass along redshift and optical luminosity bins. In addition, we find that radio-loud quasars at lower optical luminosities tend to have on average higher FIR and 250-micron luminosity with respect to radio-quiet quasars with the same optical luminosites. Even if we use a two-temperature grey-body model to describe the FIR data, the FIR luminosity excess remains at lower optical luminosities. These results suggest that powerful radio jets are associated with star formation especially at lower accretion rates., Comment: Accepted for publication in MNRAS, 17 pages, 5 figures, 5 tables

Published
2014
Full Text
View/download PDF

7. Star formation in high-redshift quasars: excess [O II] emission in the radio-loud population

Author

Kalfountzou, E., Jarvis, M. J., Bonfield, D. G., and Hardcastle, M. J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the [O II] emission line properties of 18,508 quasars at z<1.6 drawn from the Sloan Digital Sky Survey (SDSS) quasar sample. The quasar sample has been separated into 1,692 radio-loud and 16,816 radio-quiet quasars (RLQs and RQQs hereafter) matched in both redshift and i'-band absolute magnitude. We use the [O II]\lambda3726+3729 line as an indicator of star formation. Based on these measurements we find evidence that star-formation activity is higher in the RLQ population. The mean equivalent widths (EW) for [O II] are EW([O II])_RL=7.80\pm0.30 \AA, and EW([O II])_RQ=4.77\pm0.06 \AA, for the RLQ and RQQ samples respectively. The mean [O II] luminosities are \log[L([O II])_RL/W]=34.31\pm0.01 and \log[L([O II])_RQ/W]=34.192\pm0.004 for the samples of RLQs and RQQs respectively. Finally, to overcome possible biases in the EW measurements due to the continuum emission below the [O II] line being contaminated by young stars in the host galaxy, we use the ratio of the [O II] luminosity to rest-frame i'-band luminosity, in this case, we find for the RLQs \log[L([O II])_RL/L_opt]=-3.89\pm0.01 and \log[L([O II])_RQ/L_opt]=-4.011\pm0.004 for RQQs. However the results depend upon the optical luminosity of the quasar. RLQs and RQQs with the same high optical luminosity \log(L_opt/W)>38.6, tend to have the same level of [O II] emission. On the other hand, at lower optical luminosities \log(L_opt/W)<38.6, there is a clear [O II] emission excess for the RLQs. As an additional check of our results we use the [O III] emission line as a tracer of the bolometric accretion luminosity, instead of the i'-band absolute magnitude, and we obtain similar results. Radio jets appear to be the main reason for the [O II] emission excess in the case of RLQs. In contrast, we suggest AGN feedback ensures that the two populations acquire the same [O II] emission at higher optical luminosities., Comment: 12 pages, 9 figures, accepted for publication in MNRAS

Published
2012
Full Text
View/download PDF

8. EFOSC2 Spectroscopy of SWIRE-CDFS Galaxies

Author

Kalfountzou, E., Trichas, M., Rowan-Robinson, M., Clements, D., Babbedge, T., and Seiradakis, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the optical spectra of a sample of 34 SWIRE-CDFS sources observed with EFOSC2 on the ESO 3.6m Telescope. We have used the spectra and spectroscopic redshifts to validate our photometric redshift codes and SED template fitting methods. 12 of our sources are Infrared Luminous Galaxies. Of these, five belong to the class of ULIRGs and one to the class of HLIRGs with evidence of both an AGN and starburst component contributing to their extreme infrared luminosity for 3, starburst contributing for 1 and AGN contributing for 2 of them., Comment: 14 pages, 11 figures, 4 tables, accepted for publication in MNRAS

Published
2010
Full Text
View/download PDF

10. changing-look AGN NGC 1566 in quiescence with XMM-Newton: a nuclear starburst and an AGN competing in power?

Author

Tomás, L, Matzeu, G A, Jiménez Bailón, E, Kalfountzou, E, Santos-Lleó, M, Parker, M L, Ballo, L, Loiseau, N, Ehle, M, Rodríguez-Pascual, P, and González-Riestra, R

Subjects
SEYFERT galaxies, ACTIVE galactic nuclei, X-ray imaging, GALACTIC evolution, SOFT X rays, STAR formation, IONIZED gases, STARBURSTS
Abstract

Star formation accretion on to the super massive black holes (SMBHs) and feedback processes link the evolution of galaxies with their SMBHs. X-ray observations in the imaging and spectral regime have revealed to be an important tool to study the connection between nuclear activity and circumnuclear star formation in nearby active galactic nuclei (AGN). X-ray spectral diagnostics can lead to disentangle, which is the ionization mechanism in the central kiloparsecs of nearby AGN. In this paper, we investigate, by means of XMM-Newton observations, the nuclear X-ray emission of the changing-look AGN NGC 1566 during its quiescent state. European Photon Imaging Camera (EPIC) soft X-ray images show an extended arm-like morphology. A detailed analysis of the high-resolution Reflection Grating Spectrometer (RGS) and medium resolution EPIC spectra shows that the material concentrated in the central kiloparsecs region is not in the photoionization-dominated regime while the presence of collisionally ionized plasma is needed to explain the observed spectral features. In the inner region (∼1.5 kpc), the brightness of the collisionally ionized gas is comparable to the brightness of the photoionized gas: the inner region hosts a luminous starburst whose ionized gas shows up bright in the X-rays when the AGN is in quiescence. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
View/download PDF

14. The XXL survey: First results and future

Author

Pierre, M., primary, Adami, C., additional, Birkinshaw, M., additional, Chiappetti, L., additional, Ettori, S., additional, Evrard, A., additional, Faccioli, L., additional, Gastaldello, F., additional, Giles, P., additional, Horellou, C., additional, Iovino, A., additional, Koulouridis, E., additional, Lidman, C., additional, Le Brun, A., additional, Maughan, B., additional, Maurogordato, S., additional, McCarthy, I., additional, Miyazaki, S., additional, Pacaud, F., additional, Paltani, S., additional, Plionis, M., additional, Reiprich, T., additional, Sadibekova, T., additional, Smolcic, V., additional, Snowden, S., additional, Surdej, J., additional, Tsirou, M., additional, Vignali, C., additional, Willis, J., additional, Alis, S., additional, Altieri, B., additional, Baran, N., additional, Benoist, C., additional, Bongiorno, A., additional, Bremer, M., additional, Butler, A., additional, Cappi, A., additional, Caretta, C., additional, Ciliegi, P., additional, Clerc, N., additional, Corasaniti, P. S., additional, Coupon, J., additional, Delhaize, J., additional, Delvecchio, I., additional, Democles, J., additional, Desai, Sh., additional, Devriendt, J., additional, Dubois, Y., additional, Eckert, D., additional, Elyiv, A., additional, Farahi, A., additional, Ferraril, C., additional, Fotopoulou, S., additional, Forman, W., additional, Georgantopoulos, I., additional, Guglielmo, V., additional, Huynh, M., additional, Jerlin, N., additional, Jones, Ch., additional, Lavoie, S., additional, Le Fevre, J.‐P., additional, Lieu, M., additional, Kilbinger, M., additional, MaruIli, F., additional, Mantz, A., additional, McGee, S., additional, Melin, J.‐B., additional, Melnyk, O., additional, Moscardini, L., additional, Novak, M., additional, Piconcelli, E., additional, Poggianti, B., additional, Pomarede, D., additional, Pompei, E., additional, Ponman, T., additional, Ramos Ceja, M. E., additional, Rana, P., additional, Rapetti, D., additional, Raychaudhury, S., additional, Ricci, M., additional, Rottgering, H., additional, Sahlen, M., additional, Sauvageot, J.‐L., additional, Schimd, C., additional, Sereno, M., additional, Smith, G.P., additional, Umetsu, K., additional, Valageas, P., additional, Valotti, A., additional, Valtchanov, I., additional, Veropalumbo, A., additional, Ascaso, B., additional, Barnes, D., additional, De Petris, M., additional, Durret, F., additional, Donahue, M., additional, Ithana, M., additional, Jarvis, M., additional, Johnston‐Hollitt, M., additional, Kalfountzou, E., additional, Kay, S., additional, La Franca, F., additional, Okabe, N., additional, Muzzin, A., additional, Rettura, A., additional, Ricci, F., additional, Ridl, J., additional, Risaliti, G., additional, Takizawa, M., additional, Thomas, P., additional, and Truong, N., additional

Published
2017
Full Text
View/download PDF

15. The XXL survey : First results and future

Author

Pierre, M., Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Le Brun, A., Maughan, B., Maurogordato, S., McCarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh, Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferraril, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Le Fevre, J. -P, Lieu, M., Kilbinger, M., MaruIli, F., Mantz, A., McGee, S., Melin, J. -B, Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Rana, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, Martin, Sauvageot, J. -L, Schimd, C., Sereno, M., Smith, G. P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Pierre, M., Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Le Brun, A., Maughan, B., Maurogordato, S., McCarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh, Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferraril, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Le Fevre, J. -P, Lieu, M., Kilbinger, M., MaruIli, F., Mantz, A., McGee, S., Melin, J. -B, Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Rana, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, Martin, Sauvageot, J. -L, Schimd, C., Sereno, M., Smith, G. P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., and Truong, N.

Abstract

The XXL survey currently covers two 25 deg(2) patches with XMM observations of similar to 10 ks. We summarize the scientific results associated with the first release of the XXL dataset, which occurred in mid-2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z < 2) cluster, (z < 4) active galactic nuclei (AGN), and cosmic background survey science will then benefit from an extraordinary data reservoir. This, combined with deep multi-lambda observations, will lead to solid standalone cosmological constraints and provide a wealth of information on the formation and evolution of AGN, clusters, and the X-ray background. In particular, it will offer a unique opportunity to pinpoint the z > 1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions.

Published
2017
Full Text
View/download PDF

16. The XXL survey: First results and future

Author

Pierre, M, Adami, C, Birkinshaw, M, Chiappetti, L, Ettori, S, Evrard, A, Faccioli, L, Gastaldello, F, Giles, P, Horellou, C, Iovino, A, Koulouridis, E, Lidman, C, Le Brun, A, Maughan, B, Maurogordato, S, McCarthy, I, Miyazaki, S, Pacaud, F, Paltani, S, Plionis, M, Reiprich, T, Sadibekova, T, Smolcic, V, Snowden, S, Surdej, J, Tsirou, M, Vignali, C, Willis, J, Alis, S, Altieri, B, Baran, N, Benoist, C, Bongiorno, A, Bremer, M, Butler, A, Cappi, A, Caretta, C, Ciliegi, P, Clerc, N, Corasaniti, P S, Coupon, J, Delhaize, J, Delvecchio, I, Democles, J, Desai, Shantanu, Devriendt, J, Dubois, Y, Eckert, D, Elyiv, A, Farahi, A, Ferraril, C, Fotopoulou, S, Forman, W, Georgantopoulos, I, Guglielmo, V, Huynh, M, Jerlin, N, Jones, Ch, Lavoie, S, Le Fevre, J P, Lieu, M, Kilbinger, M, MaruIli, F, Mantz, A, McGee, S, Melin, J B, Melnyk, O, Moscardini, L, Novak, M, Piconcelli, E, Poggianti, B, Pomarede, D, Pompei, E, Ponman, T, Ramos Ceja, M E, Rana, P, Rapetti, D, Raychaudhury, S, Ricci, M, Rottgering, H, Sahlen, M, Sauvageot, J L, Schimd, C, Sereno, M, Smith, G P, Umetsu, K, Valageas, P, Valotti, A, Valtchanov, I, Veropalumbo, A, Ascaso, B, Barnes, D, De Petris, M, Durret, F, Donahue, M, Ithana, M, Jarvis, M, Johnston-Hollitt, M, Kalfountzou, E, Kay, S, La Franca, F, Okabe, N, Muzzin, A, Rettura, A, Ricci, F, Ridl, J, Risaliti, G, Takizawa, M, Thomas, P, Truong, N, Pierre, M, Adami, C, Birkinshaw, M, Chiappetti, L, Ettori, S, Evrard, A, Faccioli, L, Gastaldello, F, Giles, P, Horellou, C, Iovino, A, Koulouridis, E, Lidman, C, Le Brun, A, Maughan, B, Maurogordato, S, McCarthy, I, Miyazaki, S, Pacaud, F, Paltani, S, Plionis, M, Reiprich, T, Sadibekova, T, Smolcic, V, Snowden, S, Surdej, J, Tsirou, M, Vignali, C, Willis, J, Alis, S, Altieri, B, Baran, N, Benoist, C, Bongiorno, A, Bremer, M, Butler, A, Cappi, A, Caretta, C, Ciliegi, P, Clerc, N, Corasaniti, P S, Coupon, J, Delhaize, J, Delvecchio, I, Democles, J, Desai, Shantanu, Devriendt, J, Dubois, Y, Eckert, D, Elyiv, A, Farahi, A, Ferraril, C, Fotopoulou, S, Forman, W, Georgantopoulos, I, Guglielmo, V, Huynh, M, Jerlin, N, Jones, Ch, Lavoie, S, Le Fevre, J P, Lieu, M, Kilbinger, M, MaruIli, F, Mantz, A, McGee, S, Melin, J B, Melnyk, O, Moscardini, L, Novak, M, Piconcelli, E, Poggianti, B, Pomarede, D, Pompei, E, Ponman, T, Ramos Ceja, M E, Rana, P, Rapetti, D, Raychaudhury, S, Ricci, M, Rottgering, H, Sahlen, M, Sauvageot, J L, Schimd, C, Sereno, M, Smith, G P, Umetsu, K, Valageas, P, Valotti, A, Valtchanov, I, Veropalumbo, A, Ascaso, B, Barnes, D, De Petris, M, Durret, F, Donahue, M, Ithana, M, Jarvis, M, Johnston-Hollitt, M, Kalfountzou, E, Kay, S, La Franca, F, Okabe, N, Muzzin, A, Rettura, A, Ricci, F, Ridl, J, Risaliti, G, Takizawa, M, Thomas, P, and Truong, N

Abstract

The XXL survey currently covers two 25 deg(2) patches with XMM observations of similar to 10 ks. We summarize the scientific results associated with the first release of the XXL dataset, which occurred in mid-2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z < 2) cluster, (z < 4) active galactic nuclei (AGN), and cosmic background survey science will then benefit from an extraordinary data reservoir. This, combined with deep multi-lambda observations, will lead to solid standalone cosmological constraints and provide a wealth of information on the formation and evolution of AGN, clusters, and the X-ray background. In particular, it will offer a unique opportunity to pinpoint the z > 1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions.

Published
2017

17. Evidence that the AGN dominates the radio emission in z ~ 1 radio-quiet quasars

Author

White, Sarah, Jarvis, M., Kalfountzou, E., Hardcastle, M., Verma, A., Cao Orjales, J., Stevens, J., White, Sarah, Jarvis, M., Kalfountzou, E., Hardcastle, M., Verma, A., Cao Orjales, J., and Stevens, J.

Abstract

© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.In order to understand the role of radio-quiet quasars (RQQs) in galaxy evolution, we must determine the relative levels of accretion and star-formation activity within these objects. Previous work at low radio flux densities has shown that accretion makes a significant contribution to the total radio emission, in contrast with other quasar studies that suggest star formation dominates. To investigate, we use 70 RQQs from the Spitzer-Herschel Active Galaxy Survey. These quasars are all at z ~ 1, thereby minimizing evolutionary effects, and have been selected to span a factor of ~100 in optical luminosity, so that the luminosity dependence of their properties can be studied. We have imaged the sample using the Karl G. Jansky Very Large Array (JVLA), whose high sensitivity results in 35 RQQs being detected above 2s. This radio data set is combined with far-infrared luminosities derived from grey-body fitting to Herschel photometry. By exploiting the far-infrared-radio correlation observed for star-forming galaxies, and comparing two independent estimates of the star-formation rate, we show that star formation alone is not sufficient to explain the total radio emission. Considering RQQs above a 2s detection level in both the radio and the far-infrared, 92 per cent are accretion dominated, and the accretion process accounts for 80 per cent of the radio luminosity when summed across the objects. The radio emission connected with accretion appears to be correlated with the optical luminosity of the RQQ, whilst a weaker luminosity dependence is evident for the radio emission connected with star formation.

Published
2017

19. Herschel-ATLAS★: far-infrared properties of radio-loud and radio-quiet quasars

Author

Kalfountzou, E., primary, Stevens, J. A., additional, Jarvis, M. J., additional, Hardcastle, M. J., additional, Smith, D. J. B., additional, Bourne, N., additional, Dunne, L., additional, Ibar, E., additional, Eales, S., additional, Ivison, R. J., additional, Maddox, S., additional, Smith, M. W. L., additional, Valiante, E., additional, and de Zotti, G., additional

Published
2014
Full Text
View/download PDF

22. The largest X-ray-selected sample of z > 3 AGNs: C-COSMOS and ChaMP.

Author

Kalfountzou, E., Civano, F., Elvis, M., Trichas, M., and Green, P.

Subjects
GALACTIC redshift, ACTIVE galactic nuclei, STELLAR evolution, CLASSIFICATION, LUMINOSITY distance, STELLAR luminosity function
Abstract

We present results from an analysis of the largest high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) sample to date, combining the Chandra Cosmological Evolution Survey and Chandra Multi-wavelength Project surveys and doubling the previous samples. The sample comprises 209 X-ray-detected AGNs, over a wide range of rest-frame 2-10 keV luminosities log LX = 43.3-46.0 erg s-1. X-ray hardness rates show that ~39 per cent of the sources are highly obscured, NH > 1022 cm-2, in agreement with the ~37 per cent of type-2 AGNs found in our sample based on their optical classification. For ~26 per cent of objects have mismatched optical and X-ray classifications. Utilizing the 1/Vmax method, we confirm that the comoving space density of all luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~ 7. With a significant sample of AGNs (N = 27) at z > 4, it is found that both source number counts in the 0.5-2 keV band and comoving space density are consistent with the expectation of a luminosity-dependent density evolution (LDDE) model at all redshifts, while they exclude the luminosity and density evolution (LADE) model. The measured comoving space density of type-1 and type-2 AGNs shows a constant ratio between the two types at z > 3. Our results for both AGN types at these redshifts are consistent with the expectations of LDDE model. [ABSTRACT FROM AUTHOR]

Published
2014
Full Text
View/download PDF

23. The XXL survey: first results and future

Author

Pierre, M., Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Brun, A. Le, Maughan, B., Maurogordato, S., McCarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferrari, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Fevre, J. -P. Le, Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., McGee, S., Melin, J. -B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Ranalli, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, M., Sauvageot, J. -L., Schimd, C., Sereno, M., Smith, G. P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Bristol [Bristol], Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Bologna (OABO), University of Michigan [Ann Arbor], University of Michigan System, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Anglo-Australian Observatory (AAO), Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), University of Liverpool, National Astronomical Observatory of Japan (NAOJ), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Physics [Thessaloniki], Aristotle University of Thessaloniki, Argelander-Institut für Astronomie (AlfA), University of Zagreb, NASA Goddard Space Flight Center (GSFC), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, University of Victoria [Canada] (UVIC), Istanbul University, European Space Astronomy Centre (ESAC), European Space Agency (ESA), INAF - Osservatorio Astronomico di Roma (OAR), Department of Physics [Oxford], University of Oxford [Oxford], Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Indian Institute of Technology [Hyderabad] (IIT Hyderabad), University of Geneva [Switzerland], Uppsala University, INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), The University of Western Australia (UWA), University of Bologna, University of Chicago, University of Birmingham [Birmingham], CEA, DSM, SPP, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INAF - Osservatorio Astronomico di Padova (OAPD), European Southern Observatory (ESO), Lund University [Lund], University of Colorado [Boulder], Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Yamagata University, Victoria University of Wellington, Roma Tre University, Hiroshima University, York University [Toronto], Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Sussex, Università degli Studi di Roma Tor Vergata [Roma], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), National Observatory of Athens, Institute for Space Applications and Remote Sensing, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, Università degli Studi di Roma 'La Sapienza' [Rome], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Pierre, M, Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Le Brun, A., Maughan, B., Maurogordato, S., Mccarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P.S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferraril, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Le Fevre, J.-P., Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., Mcgee, S., Melin, J.-B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ramos Ceja, M.E., Rana, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlen, M., Sauvageot, J.-L., Schimd, C., Sereno, M., Smith, G.P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Corasaniti, P. S., Desai, S. h., Jones, C. h., Le Fevre, J. P., Maruili, F., Melin, J. B., Ramos Ceja, M. E., Sauvageot, J. L., Smith, G. P., Johnston Hollitt, M., LA FRANCA, Fabio, Ricci, Federica, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, Université de Genève = University of Geneva (UNIGE), Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), Harvard University-Smithsonian Institution, University of Bologna/Università di Bologna, Universiteit Leiden, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: active, X-ray: general, FOS: Physical sciences, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, XXL survey, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], clusters: general [galaxies], cosmological parameter, X-ray:general, cosmological parameters, general [X-ray], QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB
Abstract

The XXL survey currently covers two 25 sq. deg. patches with XMM observations of ~10ks. We summarise the scientific results associated with the first release of the XXL data set, that occurred mid 2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions., Proceeding of the XMM Next Decade Workshop held at ESAC, 9-11 May 2016

Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results