OSIRIS Guaranteed Time - Reserved Targets

The Luminosity Function of High Redshift Galaxies through Gravitational Lensing

PI: José Antonio de Diego

ABSTRACT

Study of the luminosity funtion (LF) of high redshift galaxies and Ly-alpha emitters. We will sweep the spectrum with narrow band images (FWHM∼12 A) using the GTC-OSIRIS tunable filters to enhance the contrast to detect emission line galaxies. Adding up the exposures we will obtain also broad band imaging useful to detect the continuum of non line emitting galaxies. The observational fields will be centered on modeled gravitational lens clusters of galaxies, to take advantage from the lens magnification to investigate the faint tail of the LF. The data will be used to study galaxy evolution, dark matter and baryonic distributionin the lens-cluster, and to improve the gravitational lens models.

TARGETS

Target Name RA(2000) Dec(2000) z
MS 2053.7-0449 20 56 22.4 -04 37 43 0.583

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Extragalactic black holes: are ULXs intermediate mass black holes?

PI: Jorge Casares Velázquez

ABSTRACT

The nature of ULXs in nearby galaxies is highly controversial: are they the long-sought intermediate mass black holes or a new state of stellar-mass black hole X-ray binary? Only radial velocity studies can unambiguously solve this puzzle, and we have chosen the brightest ULXs (B≤22) in NGC 5204 and Holmberg II accessible to GTC. We propose long-slit spectroscopy with OSIRIS to obtain the first radial velocity curve of a ULX companion star and probe whether they contain ∼100 - 1000 MSUN black holes or not. In addition, we plan to test whether IC 10 X-1 (with a WR donor) hosts the most massive extragalactic binary black hole.

TARGETS

Target Name RA(2000) Dec(2000)
IC 10 X-1 00 20 29.1 +59 16 51
Holmberg II ULX 08 19 29.0 +70 42 19.3
NGC 5204 ULX 13 29 38.6 +58 25 05.7

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The evolution of the Lyα emitters from z = 0.3 to z = 4

PI: Jordi Cepa

ABSTRACT

HORUS (Hydrogen and Oxygen Recombination lines Unified Survey) is aimed at building a representative and homogeneus sample of Lyα sources (Lyα blobs and Lyα emitters -LAEs-) in the sensitive redshift domain z∼2-4. For this Guaranteed Time proposal, the redshift z=2.1 has been selected as pilot survey for HORUS. This redshift will be scanned in depth using the OSIRIS tunable filter (TF) tomography, an innovative technique for 8-10m telescopes that makes HORUS a truly unique project. It allows a direct selection of objects by their Lyα emission. The Lyα luminosities, equivalent widths, morphologies and velocity dispersions obtained, will allow to study the evolution of the LAEs luminosity function, large scale structures and clustering, to compare with our model predictions and Dark Matter distributions.

TARGETS

Target Name RA(2000) Dec(2000)
EGS 14 16 35 +52 16 25
SSA22 22 17 06 +00 17 00
SXDS 02 18 00 -05 00 00

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The impact of metallicity on massive star evolution

PI: Artemio Herrero

ABSTRACT

Metallicity plays a key role in the physics of the Universe, particularly in the structure and evolution of stars and galaxies. Local Group galaxies cover a large range in metallicity, and we can observe and analyze individually their most luminous stars to determine stellar parameters and abundances (mainly C, N, O and alpha-elements, but also Fe-group abundances in some cases) as a function of metallicity and galactic position. We apply for Multi-Object Spectroscopy of blue massive stars in nearby galaxies of the Local Group (Sextans A, M31 and M33) that range a factor of 30 in metallicity. This way we will test current theories about the winds and evolution of massive stars and their dependence with metallicity.

TARGETS

Target Name RA(2000) Dec(2000)
Sextans A 10 11 05.70 -04 42 28.0
M31-CENTER 00 42 44.31 +41 16 09.4
M33-CENTER 01 33 51.02 +30 39 36.7
M33-1 01 33 51.02 +30 39 36.7
M33-2 01 33 51.02 +30 39 36.7

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A TF Study of evolution of galaxies in clusters

PI: Miguel Sánchez Portal

ABSTRACT

GLACE (GaLAxy Cluster Evolution Survey) is an innovative deep panoramic OSIRIS tunable-filter survey of [Oii]3727, [Oiii]5007, Hβ and Hα/[Nii]6584 in several clusters at z=0.40, ∼0.65 and 0.89. It is aimed to study the variation of galaxy properties (star formation, AGN activity and morphology) as a function of environment in a representative and uniquely well-studied sample of clusters, adddressing key questions about the physical processes acting upon the infalling galaxies during the course of hierarchical growth of clusters. For this Guaranteed Time proposal, one cluster at z∼0.40 has been selected as a pilot survey for GLACE. Extensive multiwavelength data already available (redshifts, multi-colour broadband imaging, X-ray, mid-IR etc.) will be exploited.

TARGETS

Target Name RA(2000) Dec(2000)
ZwCI 0024.0+1652 00 26 36.0 +17 08 36

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Emission line maps and gas properties of a giant star formation

PI: Emilio Alfaro

ABSTRACT

We propose to get detailed maps of gas properties in a young stellar super-complex located in the galaxy NGC 6946 which harbours a super star cluster (SSC) around 15 Myr old, with an estimated mass above some 106 MSUN. To this aim we will make use of the unique capabilities provided by OSIRIS + GTC for getting narrow-band differential images centred at some specific emission lines. The analysis of these maps will provide important clues about the interaction between massive young stars (stellar winds, SN explosions, UV radiation, etc...) and gas properties in this kind of extended and massive star formation region. The combination OSIRIS+GTC in the ideal instrument, in terms of spatial coverage sensitivity and spectral and spatial resolution, for performing this kind of study.

TARGETS

Target Name RA(2000) Dec(2000) Type
NGC 6946-1347 20 34 32.03 +60 08 14.7 Giant Star Forming Region

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A Tunable-Filter study of Blue Compact Dwarf Galaxies

PI: Hector Castañeda

ABSTRACT

We propose to study a sample of Blue Compact Dwarf (BCD) galaxies using the Tunable Filters of OSIRIS at the 10.4m GTC. The optical data will produce images in the wavelengths of Hα, Hβ, [NeIII]λ3869, [OII]λ3727, [OIII]λ4363 and λ5007, [NII]λ5755 and λ6584, Heλ6678, [SII]λ6717 and λ6731, [SIII] 9069, as well as the WR emission features at λλ4850-4686 and λλ5698-5808. The high-quality data will provide us with an unprecedent set of images for this kind of objects that will allow to determine the amount, extension and shape of ionized gas at high and low surface brigthnesses, the extinction maps, the global and local star formation rate, the electron density and temperature spatial distribution, the spatial variations in the chemical composition and the precise localization of the WR stars.

TARGETS

Target Name RA(2000) Dec(2000)
hs0017+1055 00 20 21.40 +11 12 21.0
hs0052+2536 00 54 56.40 +25 53 08.0
hs0052+2537 00 54 56.00 +25 53 23.0
um311 01 15 34.40 +07 59 24.0
hs0122+0743 01 25 34.20 +07 59 24.0
um133 01 44 41.28 +04 53 26.0
um382 01 58 09.42 -00 06 38.3
ugca20 01 43 14.72 +19 58 31.7
sbs0335-052e 03 37 38.40 -05 02 36.0
mrk1089 05 01 37.81 -04 15 29.8
mrk1090 05 01 44.01 -04 17 19.5
iizw40 05 55 42.63 +03 23 31.0
hs0749+582 07 53 51.25 +58 08 09.8
hs0822+3542 08 25 55.43 +35 32 31.9
he2-10 08 36 15.18 -26 24 33.9
ugc04483 08 37 03.00 +69 46 31.0
izw18 09 34 02.03 +55 14 28.1
sbs0940+544 09 44 16.72 +54 11 32.9
sbs0943+561 09 46 46.57 +55 57 04.6
haro2 10 32 31.93 +54 24 03.5
Tol 9 10 34 38.70 -28 35 00.0
sbs1116+597 11 18 47.53 +59 26 00.0
viizw403 11 27 59.90 +78 59 38.9
sbs1128+573 11 31 16.51 +57 04 00.4
mrk1450 11 38 35.62 +57 52 27.2
um461 11 51 33.04 -02 22 22.8
sbs1159+545 12 02 02.44 +54 15 50.1
sbs1211+540 12 14 02.50 +53 45 18.0
tol1214-277 12 17 17.09 -28 02 32.7
hs1222+3741 12 24 36.73 +37 24 36.2
mrk0209 12 26 16.02 +48 29 36.6
sbs1249+493 12 51 52.53 +49 03 26.9
hs1236+3937 12 39 20.14 +39 21 04.8
Tol 30 13 05 46.70 -28 25 20.0
hs1304+3529 13 06 24.24 +35 13 41.6
hs1318+3239 13 21 03.26 +32 24 16.2
hs1319+3224 13 21 19.92 +32 08 23.0
pox186 13 25 50.67 -11 37 34.9
hs1330+3651 13 33 08.28 +36 36 33.1
hs1347+3811 13 49 12.35 +37 56 44.1
sbs1415+437 14 17 01.76 +43 30 13.4
hs1424+3836 14 26 28.07 +38 22 59.1
hs1442+4250 14 44 12.10 +42 37 37.0
sbs1533+574b 15 34 14.35 +57 17 01.2
hs2352+2733 23 54 56.70 +27 49 59.0

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The OTELO survey

PI: Jordi Cepa

ABSTRACT

OTELO (OSIRIS Tunable Emission Line Object Survey), will survey emission line objects using OSIRIS tunable filters in selected atmospheric windows relatively free of sky emission lines. Different high latitude and low extinction sky regions with enough angular separations will be observed yielding a total area of 0.1 square degrees. A 3σ depht of 2x10-18erg cm2s-1 will allow detecting objects of EW∼3 at this flux limit, making OTELO the deepest emission line survey to date. OTELO is a deep space probe that will provide a representative sample of the Universe from z=0.24 through 6.7 to study, with un precedent detail, the evolution of emission line galaxies. Since the observing procedure will make use of the Tunable Filter Tomography OTELO will allow studying clearly defined volumes of Universe at a known flux limit.

TARGETS

Target Name RA(2000) Dec(2000)
COSMOS 10 00 29 +02 12 21
GOODS-N 12 36 49 +62 12 58
EGS 14 16 35 +52 16 25
SXDS 02 18 00 -05 00 00

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The impact of the host galaxy environment to trigger SNe and GRBs: probing the SN factory NGC2770

PI: Alberto J. Castro-Tirado

ABSTRACT

It is well known that long Gamma-Ray Bursts (GRBs) are created by the explosion of massive stars, showing similarities with Supernovae (SNe). The recent discovery of X-ray bursts in a few SNe (called X-ray flashes, XRFs), makes the frontier between SNe and GRBs even more diffuse. These findings support a unified model where SNe-XRFs-GRBs would be explained just by different physical-chemical properties of the collapsing star (mass, angular momentum, metallicity). The SN factory, NGC2770, showed in the last 9 years 2 SNe and 1 XRF, making it an ideal laboratory to study the environment impact to trigger a SN or/and an XRF. Our final goal is to derive a star-formation-rate/extinction/metallicity/shocked-material map of NGC2770, specially at the regions where the explosive events occurred.

TARGETS

Target Name RA(2000) Dec(2000)
NGC2770 09 09 33.62 +33 07 24.6

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Where do the disks of spiral galaxies end?

PI: Joss Bland-Hawthorn

ABSTRACT

Until recently, it was thought that all spiral disks truncate close to the Holmberg radius (26.5 mag arcsec-2), but this belief was based on surface photometry. Resolved stellar population studies reach down to much lower effective surface brightness levels, and have now shown that three stellar disks (Galaxy, M31, NGC 300) in fact show no evidence of truncation. Moreover, the declining [Fe/H] abundance gradient in all three galaxies flattens off in the outer disk which was unexpected. We propose to trace the outer stellar disks of two of the best northern objects, NGC 628 and NGC 2403, and to determine their outer abundance gradients beyond the current radial extremes.

TARGETS

Target Name RA(2000) Dec(2000)
NGC 628 01 36 41.8 +15 47 00
NGC 2403 07 36 51.4 +65 36 09

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How do galaxies get their gas?

PI: Joss Bland-Hawthorn

ABSTRACT

HI observations of nearby disk galaxies reveal a serious shortfall in the gas accretion rate to account for the star formation history (roughly 1 - 3 solar masses per year). This indicates that much of the accreted gas coming through the halo is in a warmer state (104-5.3 K) and at suffciently low emission measure (< 1 cm-6 pc) that it would have been missed in past observations. We propose to carry out the deepest Hα, [NII] and [OIII] imaging to date for two nearby galaxies that are useful surrogates for the Galaxy. We will search for ionized gas beyond the HI disk edges and at high galactic latitudes. The line ratio maps ([NII]/Hα, [OIII]/Hα) will shed light on whether the gas is part of an inflow or an out flow.

TARGETS

Target Name RA(2000) Dec(2000)
NGC 891 02 22 33.4 +42 20 57
NGC 3198 10 19 54.9 +45 32 59

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Radiative Feedback in the Early Universe

PI: Joss Bland-Hawthorn

ABSTRACT

We propose exploratory observations for a future large programme dedicated to the study of emission-line gas and galaxies in the vicinity of the most powerful quasars at z ∼ 2 - 3. We propose to observe the vicinity of 2 of the most luminous UV-bright quasars (+ a control sample of 2 less luminous quasars). We will observe exclusively in the B band where the sky is darkest to ensure the deepest sensitivity to weak Lyα emitting gas. This experiment has only been attempted for a single luminous quasar to date (> 1047 erg s-1) and remarkably no emission-line gas or galaxies were detected in the vicinity of the source. This may suggest that there is a critical flux level at which radiative feedback seriously alters the physical state of the environment and suppresses star formation.

TARGETS

Target Name RA(2000) Dec(2000)
Sources all over sky

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Narrow-band Ly-alpha imaging of a selected sample of high-redshift (z > 2) gamma-ray burst host galaxies

PI: Alberto J. Castro-Tirado

ABSTRACT

About 100 gamma-ray burst (GRB) host galaxies have been detected since the discovery of the GRB afterglows in 1997. In general, most GRB host galaxies are actively star-forming, characterised by restframe UV emission and large emission-line equivalent widths. We propose to obtain Lyα narrow-band images of a reduced sample 6 GRB host galaxies in the redshift range 2 < z < 6. They have been selected from a larger sample (containing 28 galaxies) which includes all GRB hosts detected so far for z > 3. Lyman-α imaging is a probe of the star formation rate and dust content of GRB host galaxies. In addition to that, it will be a way to probe if the host galaxy resides in an overdense environment.

TARGETS

Target Name RA(2000) Dec(2000)
GRB050904 00 54 51.30 +14 05 09.7
GRB021004 00 26 54.69 +18 55 41.3
GRB971214 11 56 25.20 +65 11 57.9
GRB030115 11 18 30.55 +15 03 57.7
GRB030323 11 06 09.38 -21 46 13.3
GRB060121 09 09 52.13 +45 39 44.9
GRB060927 21 58 11.93 +05 21 50.3
GRB050814 17 36 45.39 +46 20 21.6
GRB060522 21 31 44.82 +02 53 10.4
GRB060707 23 48 19.00 -17 54 17.0
GRB050730 14 08 17.14 -03 46 17.8
GRB060510B 15 56 29.61 +78 34 13.0
GRB060223 03 30 49.74 -17 07 48.0
GRB050505 09 27 03.30 +30 16 23.7
GRB060206 13 31 43.40 +35 02 59.9
GRB060210 03 50 57.41 +27 01 34.4
GRB050502 13 39 46.25 +42 40 27.5
GRB060115 03 36 08.40 +17 20 43.0
GRB070721B 02 12 32.97 -02 11 40.4
GRB061222B 07 01 24.77 -25 51 33.9
GRB061110B 21 35 40.40 +06 52 34.1
GRB050908 01 21 50.70 -12 57 16.0
GRB050319 10 16 47.76 +43 32 54.9
GRB060926 17 35 43.66 +13 02 18.6
GRB060906 02 43 00.9 +30 21 42.1
GRB060605 21 28 37.16 -06 03 33.8
GRB060526 15 31 18.31 +00 17 03.7
GRB020124 15 31 50.80 -11 31 11.0

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Tomography of high-redshift clusters

PI: Alberto Fernández-Soto

ABSTRACT

Clusters of galaxies are amongst the largest cosmological structures. However, not much is yet known in detail about the properties of clusters at redshifts of cosmological interest. We propose here to exploit a new method to study large samples of cluster galaxies using microslits and nod-and-shuffle to perform spectroscopy of many objects in single fields in a narrow spectral range-chosen to fit an emission line at the cluster redshift. Our objective is to obtain spectroscopy in a very restricted wavelength range (≈ 300 A in width) of up to one thousand objects for each single 8x3 square arcmin field. Many of them will be identified as cluster emission-line objects and will yield basic measurements of the dynamics and the star formation in the cluster. This proposal aims at testing this pioneering approach on a single cluster at z∼0.3.

TARGETS

Target Name RA(2000) Dec(2000)
Zw3146 10 23 39.6 +04 11 10.4

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Osiris Ultra-deep Tunable-filter Mapping of the Outer Regions of Ellipticals

PI: Alexandre vazdekis

ABSTRACT

We aim at studying the stellar populations and kinematics of elliptical galaxies and their globular cluster systems beyond their effective radii. We will apply a novel approach, specifically developed for this purpose, using absorption-line mapping technique with OSIRIS tunable filters. We will observe two representative field ellipticals of different masses to determine:

  • i) galaxy age, metallicity and [Mg/Fe] gradients to 3 re, and 2-D maps of these quantities to ∼ 1 re
  • ii) galaxy velocities/velocity dispersions to 3-4 re, and 2-D maps of these quantities to ∼ 1 re
  • iii) velocities for up to half the galaxy GCs to 10 re.

The data will allow us to study elliptical galaxy stellar populations at large radii, and for the mass distributions and orbital properties of galaxy haloes at cosmologically important galactocentric radii.

TARGETS

Target Name RA(2000) Dec(2000)
NGC0720 01 53 00.5 -13 44 19
NGC0821 02 08 21.1 +10 59 42

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Lockman SpReSO: Lockman Hole Spectroscopic Redshift Survey with OSIRIS

PI: J. Cepa (IAC) and J. González (IA-UNAM)

ABSTRACT

This proposal is aimed at the optical spectroscopic study, using the MOS mode of OSIRIS at GTC, of sources up to magnitude 24.5 in the central 30x30 arcmin of the Lockman Hole field, which has been observed with XMM at the highest depth. Within the selected objects, optical counterparts of X-ray and Spitzer 24mu sources will be specifically targeted. Some of the goals of this survey include studying the evolution of SFR and efficiencies, optical vs. FIR extinctions, metallicities, stellar populations, and specific populations of high redshift objects such as AGNs, LAEs, SMGs and ULIRGs.

TARGETS

Target Name RA(2000) Dec(2000)
Lockman 10 52 43.0 +57 28 48.0

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Last modified: 03 July 2013