HeViCS/HeFoCSSPIRE DataStatus and future releases

Extended HRS ProfilesCurrent Results

Matthew Smith

Matthew.Smith@astro.cf.ac.uk

Last Version: DR3.5

Released June 2012

Pipeline: Optimised De-glitcher BriGAdE Allow Dark Pixel drift

removal Manual Jump and

glitch-tail removal New Pixel sizes:

6, 8, 12"

HeFoCS

HeViCSV1

V2

V3

V4

Latest Version: DR4

Released June 2012

Updates from DR3.5 to DR4: PMW cal factor v5 to v8

applied to map (1.0067) Second-order deglitching Relative Gain Corrections

for extended emission

How does the standard pipeline compare?

For extra-galactic science we have optimum SPIRE pipeline (cirrus scale structures may-not be optimal)

Pointing Products Star-Tracker Temperatures were changed on

OD 320 to prevent hot-pixel issues Herschel updated on OD 761 to account for

changes New pointing products OD 320-761 available

(~ 2")

Herschel Map-Making Workshop?

Data Release 5

Planned Updates on DR4 NEW CALIBRATION!

(point + ext) New Pointing Product

Updates not going to be applied Planck Zero Level Calibration De-striper (except on a set of cirrus maps for

Simone

New Neptune measurements by George Increase of ∼3% , ∼2% & ∼1% at 250, 350 and

500µm

Aperture Efficiency values now included (fairly small)

Long term – will be new updates on the assumed Neptune and Uranus models

Point Source Calibration

Chris North, Matt Griffin, & co

Applies to fully extended until >100'

Working on adaptive script for intermediate sources 10 – 100'.

Extended Calibration

Will require TWO versions of SPIRE for point/extended or even individual object maps that are

optimised to their size

Old Philosophy – FUDGE IT: Modify the filter curve with a λ2 weighting

Wrong for 2 reasons: 1: Beam solid angle varies as λ1.7 2: Not a single value of beam area appropriate for sources

Depending on your source spectral index could correct the wrong way.

Extended Calibration (2)

Why the difference? See white board!

New Philosophy As well as apply colour–corrections account for varying

beam area across band Talking somewhere in the region 0-10% change in values

New pipeline surface brightness product in MJy/sr

Is a Planck zero level corrected map as well (but not really worth it)

Extended Calibration (3)

Nice and Simple?

The HRS & Virgo

An original aim of the HRS (and many other surveys) to find cold dust in outskirts of galaxies.

Dust could be driven out or formed outside disk.

Has been detected by quasar absorption (Menard et al. 2010) – see next slide.

Not been possible to detect emission before as dust is cold and very low surface brightness.

Still work in progress...

Extended Dust (bonus chapter!)

Potential Questions? How far can we detect dust emission What are the properties of the dust at these

wavelengths Extreme environment for SF etc…

Only used SPIRE only due to sensitivity / reduction method / areas covered

Still work in progress

Extended Dust (2)

uses SDSS

∼85,000 quasars at z > 1

Correlated with 24 million galaxies at z∼0.3

Find reddening and magnification

Half of dust is outside galaxies

Menard et al. 2010

Stacked Radial ProfilesHRS object Criteria:

• Late-type galaxies

• Indentified as detection

• Extended Source

• No other bright contaminating object

• No heavy cirrus contamination

• Inclination < 60°

Stacked Radial Profiles (2)

Restricted to galaxies with D25 > 3ˊ

Stacked Radial Profiles (3)

Have randomly chosen 32 galaxies (1/4 sample) and repeated procedure

Measured where it crosses a fixed threshold (equivalent to 1.8R25)

Repeated 40,000 times

Results do not vary by a large amount (±0.15 R25)

Monte-Carlo Tests

Probably Not!

Can other Surveys do better?

Nearby Objects

Large extended objects

Bright

Maps not large enough

Wide Field Surveys, e.g., H-ATLAS

Many objects so can be sensitive

Large areas so can reach high scales

Angular size is smaller, flux of central beam dominates at radii < 2.0R25

Minimise χ2 model by: Trial Model Convolving it with beam Calculate χ2

Following Schruba et al. 2011 do not fit centre 30˝ Need 2 exponentials

Best-Fit Model

The fraction of dust emission between 1-2 R25 is 6.6, 8.0 and 10.6% for the 250, 350 and 500µm band.

If integrate the broken-exponential model from 0⇢∞ find that 4.2% of emission at 250µm

Rough agreement with 15kpc Medard value but I need to redo this.

Stacked Radial Profiles (2)

Temperature Results Work in Progress… All images smoothed and re-gridded to

PLW images Temperature stabilises around 16K Means a higher fraction of dust mass

outside R25 than fraction 250µm emission

HIDeficienc

y Difference is less

prounonced as Cortese 2010

Individual objects are in agreement

Highly HIdef are significantly different from HIdef < 0.0 (Mann-Whitney U statistic)

Morphology Not yet

Investigated…

Stellar

Mass

Are low mass galaxies cosmic hoovers picking up dust expelled from high stellar mass galaxies?

Schruba et al. with CO with HERACLES reach 1.0-1.2R25

Other Tracers

HI Paolo Serra suggested a thesis by Thomas Martinsson

Unknown for other wavelengths (e.g., UV)?