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I also created a super fast but effective elliptical routine that I often use before hitting the weights! The Plan for the rest of the day is to head over to French class, grab some lunch, and then prepare myself for my Calculus section and 4 hour Chemistry lab (vomit). Those are some awesome shorts, Christine; in fact, I’d like to have that whole outfit! Christine is a self-proclaimed apple pie connoisseur with a small obsession with all things giraffes. January 22, 2013 by Julie 74 Comments After staring at my computer screen all morning, I started to feel rather sluggish.
I didn’t want to workout at all but knew I’d feel 10 times better – both mentally and physically – if I worked up a sweat. As always, exercise proved to be an instant mood booster and I left the gym after a lunchtime workout feeling much more motivated to tackle my to-do list for the day. I’ve been on the lookout for some new treadmill walking workouts thanks to the frigid temps we’ve been having here in SLC, so this is perfect! I agree that if you walk inclines and at different speeds, your shins, glutes, everything will slowwwly begin to burn~! I had a hard time getting out of bed this morning going to the gym, but I know my day started off to a much better start since I went.
An alternative theory to dark matter developed in 1983 by the astrophysicist Mordehai Milgrom of the Weizman institute in Israel, called the modified Newtonian dynamics (MOND) has successfully predicted the rotational properties of two elliptical galaxies formed by a different process from spiral galaxies. In the new research, Milgrom analyses the rotation curves of two elliptical galaxies and shows that the predictions of MOND --that under certain circumstances the gravitational force between two bodies decays more gently than the inverse square of the distance between them--are equally valid.
The image at the top of the page shows the center of an elliptical galaxies that has been found to emit unexpectedly high amounts of blue and ultraviolet light. In this false-color photograph by the Hubble Space Telescope, the center of nearby dwarf elliptical M32 has actually been resolved and does indeed show thousands of bright blue stars. Does MOND explain gravatational lensing around areas that don't seem to contain baryonic matter? If your overarching theory of the Cosmos is wrong (intolerable heresy, I know), then interpretations of study, and their hypothetical speculations, will probably also turn-out to be wrong, or, at best, misaligned.
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Jerry Gagnier: Had the same problem and "solved" it by removing the foot pad and lubricating every groove made by the pad on the cushioning tape underneath the pad, including the stud holes made by the pad.
The pedal squeak ultimately turned out to be the "square peg" (outside) end of the main bolt that holds the foot pedal to the arm. Mostly, I've traced noises and bump feelings to the elbow joint at the front of the machine.
In this paper, we take a look at the most crucial event in the life of a galaxy: the end of star formation. Not all stars shine the same way though: stars much more massive than our sun are very bright and shine in a blue light as they are very hot.
The received wisdom in galaxy evolution had been that spirals are blue, and ellipticals are red, meaning that spirals form new stars (or rather: convert gas into stars) and ellipticals do not form new stars (they have no gas to convert to stars).
A few years back, astronomers noticed that not all galaxies are either blue and star forming or red and dead. In the case of spirals, we see lots of blue ones, quite a few green one and then red ones (Karen Masters has written several important Galaxy Zoo papers about these red spirals). We can confirm this difference in quenching time scales by looking at the ultraviolet and optical colours of spirals and ellipticals in the green valley.
The guest post below is by Zach Pace, an undergraduate physics student at the University of Buffalo.
As many readers probably know, a galaxy’s magnitude (overall brightness in the red band, on a log scale) and a galaxy’s color (the difference between the blue magnitude and a red band) are two important quantities for determining what a galaxy might look like (and how it might evolve). One of the main goals of Zoo 2 is to gauge the extent to which morphology informs physical characteristics like color and magnitude, so my objective for the summer was to come up with good representations of color and magnitude for all of the smaller sub-populations in Zoo 2. Color-magnitude diagram (CMD) for spirals in GZ2, split by the number of spiral arms identified in each galaxy.
I also came across something unexpected when looking at bulge sizes in face-on disk galaxies.
Color-magnitude diagram (CMD) for disk galaxies in Galaxy Zoo 2, split by the relative size of the central bulge.
To fit the distributions, I used a method pioneered about 10 years ago by Ivan Baldry, which fits one parameter after another in our profile functions to find a distribution that converges onto the best fit. While it may be convenient for us to use distance units where we set a mind-blowingly large number equal to 1, it doesn’t really help us communicate our work to the public. During this hangout, we announced that your clicks and classifications of the CANDELS galaxies have been moving at such an impressive rate that the first round is finished. In the meantime, though, we’re getting ready not just to do the scientific analysis, but to share Galaxy Zoo results with our colleagues around the world. Note: although it was a beautiful sunny day in Oxford, the variable audio quality is not because I was occasionally distracted looking out the window. Spiral galaxies are seemingly endless sources of fascination, perhaps because they’re so complex and diverse.
All of the above questions are related to a question we got right at the end of our last hangout: what is the significance of the number of spiral arms? Herschel sees much longer wavelengths than HST, so its resolution isn’t as high even though it has a bigger mirror. I enjoy days where we get to use questions from the public to meander our way through the Universe. Also, these two galaxies may have roughly the same proportions between them as between the Milky Way and the Large Magellanic Cloud. We also talked about the origin and importance of dust in galaxies, and just what a green pea would look like in the Hubble data. Bonus: green peas, voorwerpjes, and planetary nebulae are just three of the phenomena that (at least in part) glow green to human eyes because of one particular frequency of light emitted by Oxygen at a certain temperature, an atomic transition seen only rarely on Earth but fairly often in the Universe. Also, did you know that dust grains are the singles bars of the atomic universe, allowing atoms to meet and combine into molecules and cooling the gas clouds they live in — which in turn helps new stars form? I’m delighted to announce that the latest paper based on Galaxy Zoo classifications was accepted to appear in the Monthly Notices of the Royal Astronomical Society earlier this week, and appears on the arxiv this morning (link). So what was new about this paper was that we combined information on the morphologies (whether or not the spiral galaxies had bars) with information on the amount of atomic hydrogen gas the galaxies contained and and our main result was that galaxies with more atomic gas in them, are less likely to have a bar.
But I want to back up a bit first and tell you about where we get this information on the atomic gas content, and why it  might be interesting. ALFALFA is a massive survey which will map the location of atomic hydrogen over basically the whole sky visible to the Arecibo radio telescope. Trends of bar fraction with atomic gas content, galaxy colour and how many stars are in a galaxy. Bar fraction against how much more or less atomic gas a galaxy has than is typical for the number of stars it has.
Anyway you can see we still see a clear trend, which demonstrates that it’s likely to be the atomic gas driving the correlation.
Here are some examples of low and high mass galaxies which are gas rich or poor and with or without bars. At the end of the paper we put forward three possible explanations for the correlation, all of which fit in with the observations we presented. To my mind the most interesting result was a hint that if a gas rich galaxy does (rarely) host a bar, it’s optically redder than similar galaxies without bars. Anyway thanks again for the classifications, and I hope the above made at least some sense! The gold standard for galaxy classification among professional astronomers is of course the Hubble classification. I should say that my choice of galaxies for the sequence owes a lot of credit to an excellent Figure illustrating galaxy morphologies in colour SDSS images which can be found in this article on Galaxy Morphology (arXiV link) written by Ron Buta from Alabama (Figure 48). The central bulge of spiral galaxy contains older, redder stars and often also contains a invisible, massive black hole.
There is obviously little to say about the structure of irregular galaxies because they are irregular. Galaxy Zoo: Hubble has a whole new branch of questions to try and help classify these clumpy galaxies. The paper itself is another variation on what should be becoming a very familiar theme for those who have followed Galaxy Zoo science: colour and shape are not the same, and tell us different things. It was known long before Galaxy Zoo that most of the star formation in our local Universe takes place in spiral galaxies, and so they tend to be blue whereas ellipticals are often red. Before we can work out what’s going on though, we have to find our red spirals, and this is trickier than it sounds. It turns out that 6% of spiral galaxies are red, which I think is higher than most would have guessed before this project.
In my next blog, I’ll look at what we do know about this mysterious population of galaxies unearthed by your hard work.
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It's such a great feeling to accomplish a health goal, so why not inspire others to do the same? Dinner will be late (around 9 or 10) and will probably revolve around Vietnamese food and a delicious iced tea with Kyle. Isn’t it funny how a good workout can make even the most sluggish day 100 times more productive?
Walking has been my exercise of choice most of my pregnancy, and you’re right, it can be no joke if you add in some speed and incline! I wish my dog was that peaceful today, I just came home to a jacket with a fresh new hole in it and my earbuds eaten, oh the joys of having a puppy!
Walking is my main form of exercise right now, and no one ever seems to believe me when I tell them how good of a workout it can be.
When I feel sluggish after a long day at the office and am not in the mood to workout, I try to remind myself of what will happen if I don’t. My dog does the same thing too, and what makes it worse is he has long, warm fur (golden retriever) that makes it even harder to get up and move around- I just want to sit and snuggle with him! It’s a nice break from running and, as you said, it’s still a challenging workout!
I for some reason can’t stand running on the treadmill, I find it much harder than outside. According to the new analysis, MOND describes the properties of two elliptical galaxies as well as dark matter.
This is important, Milgrom argues, because elliptical galaxies are thought to have evolved in a completely different way from spiral galaxies and other disc galaxies – they are thought to be formed by the collision and merging of two other galaxies. You start with small galaxies – they merge, they collide – there are explosions in the galaxies and so on and so forth.
Most blue light from spiral galaxies originates from massive young hot stars, in contrast to the red light from the old cool stars thought to compose ellipticals. The answer is probably that these blue stars are also old and glow blue, reaching relatively high temperatures by the advanced process of fusing helium, rather than hydrogen, in their cores. The last repairman that looked at it knew to sand down a weld spot (?) that was too high and then grease it. Simple: the green valley galaxies aren’t a single population of similar galaxies, but rather two completely different populations doing completely different things! On the x-axis is the optical colour, dominated by young-ish stars, while on the y-axis is a UV colour, dominated by the youngest, most short-lived stars. What we see is that spirals start becoming redder in optical colours as their star formation rate goes down, but they are still blue in the ultraviolet. This is because their star formation rate isn’t dropping slowly over time like the spirals, but rather goes to zero in a very short time. This gas comes in from their cosmological surroundings, cools down into a disk and then turns into stars.
That means it’s not enough to just shut off the gas supply, you also have to remove the gas reservoir in the galaxy. Zach worked at the University of Minnesota during the summer of 2013 through the NSF’s Research Experience for Undergraduates (REU) program.
The lines show fits to the two main populations of elliptical (red) and spiral (blue) galaxies, following the method of Baldry et al. The distribution of colors and magnitudes for galaxies are statistically similar, no matter what the number of spiral arms. Galaxies that appear to have no central bulge (top) have very different colors and luminosity than those with dominant bulges (bottom).
If I note that the galaxy images from CANDELS look a little different from the galaxies in the SDSS because the CANDELS galaxies are typically at a redshift of 2, that’s pretty meaningless. Every galaxy has enough classifications for us to get a very good sense of what its morphology is. The summer conference season is upon us, and many of us have given and are giving talks and posters at various meetings in various cities. Determining how many spiral arms a galaxy has is hard, and is often subjective — so why bother? Part of the reason spiral arm classification & count is a challenge is that it often depends on the wavelength at which you observe a galaxy. As you get to longer and longer wavelengths, you start to pick up the heat radiated by clouds of gas and dust, which are often stellar nurseries — and often trace spiral arms.
When studying other galaxies, it’s easy to get caught up in the race to discover the biggest, the smallest, the farthest and the most extreme, and forget that our own Universal neighborhood is pretty amazing too. The Horsehead Nebula is a well-known feature in the Orion star-forming complex, and the new Hubble images provide a great opportunity to learn even more about this region that has been studied for hundreds of years.
So you see more of the structure of the cloud itself, and more of where it’s thin and thick.
So stay tuned for the next hangout when we just might have a thing or two to say about dark matter, dark energy and new projects! Our latest live hangout saw us discussing the latest update to the Galaxy Zoo site — made based on your clicks!
Astronomers very broadly group stars into three populations depending on their composition. The slightly older stars, many of which are still around and living in our galaxy and others, are Population II; and the very massive rockstars of the early universe that have all died out are called Population III.
Heating and cooling, gravity and pressure, and the interplay between atoms, molecules, and radiation are all a part of what gives us this amazingly diverse Universe. What’s neat about a survey for something which emits as a specific frequency is that you actually get a 3D map of where the hydrogen is – both redshift and sky position! It represents the fuel for future star formation in a galaxy – a galaxy with a lot of atomic hydrogen could in principle make a lot of new stars. To start with correlation is not the same as causation, and to that we add that lots of things are correlated. Where a galaxy is richer in atomic hydrogen than normal it’s less likely to host a bar, and vice versa. It’s just possible that bars hold back infall of gas from the outer regions of a spiral galaxy and slow down star formation over all in that galaxy. With a few minor modifications, this classification has stood in place for almost 90 years. I strongly recommend that article if you’re looking for a thorough history of galaxy morphology. I have to say though, the Las Cumbres version of the activity looks even more fun as they also talk you through how to make your own colour images of the galaxies to put on the diagram. Each of these three broad morphologies of galaxy tells us a little about what is going on inside the galaxy itself. It is in the spiral arms that new stars are forming, hence their usually bright, blueish or white colour. This is an almost spherical fuzz of stars and globular clusters surrounding the galaxy, trapped by gravity. Dwarf galaxies might appear to be just smaller versions of the above types, but they are the most common type of galaxy. In the meantime might I suggest yet another type of galaxy, perhaps with a coffee and a bit of classification?
Not only is this another success for Galaxy Zoo science, but it’s a tribute to the hard work of Karen who led the effort. To recap slightly, as young, massive and short-lived stars are blue, colour is a measure of what’s happened recently.
In looking at the blue ellipticals and now the red spirals, it’s clear that interesting things happen when this rule is broken. If we weren’t careful, then our sample would get contaminated by edge-on systems, which appear redder because of the effect of the dust that scatters light which travels through the disk. It turns out that the greater the density of the environment a spiral finds itself in (that is, the more neighbours it has) the more likely it is to be red…but only up to a point. If it was the environment that was driving the dramatic change from blue to red, then we’d expect the properties of the red spirals to depend on the environment. Until then, if you want the gory details, you can find the latest version of the paper over here. The mid-stance heel strike during a hot shower or bath you look at your present problems that don’t fit your goal is to compete. Special K Breakfast Shakes Weight Loss America Obesity Average garcinia affiliate simple fast weight loss plan the right time importance.
It can be run once if you only need to knock off a quick 5-15 pounds or multiple times if you have more weight to lose. For the carefully selected patient with realistic expectations knee arthrodesis may relieve pain and Lack of adequate bone contact and poor stability ere cited as the main causes of failure. Share your weight loss success story with Everyday Health's Leslie Steinberg ([email protected]). Most likely, I’ll park my butt on the couch the rest of the night and get nothing done. MOND was originally formulated to describe spiral galaxies and has had singular success in predicting certain properties of these structures. MOND's success, he argues, means that its predictive accuracy cannot simply be a coincidence and that it must hint at a deeper underlying truth.
During this stormy evolution the dark matter and the normal matter are subject to these processes in very different ways and so you really do not expect to see any real correlations between the dark matter and the normal matter.
Where MOND fails is on larger scales such as in clusters of galaxies and on even larger cosmological scales.
M32 appears in many pictures as the companion galaxy to the massive Andromeda Galaxy (M31). Galaxies are the place where cosmic gas condenses and, if it gets cold and dense enough, turns into stars.

It’s those unusual objects that we started Galaxy Zoo for, and in this paper they help us piece together how, why and when galaxies shut down their star formation.
On the left: just the ellipticals (or early-types) on top and just the spirals (or late-types) on the bottom.
If you look at the colour-mass diagram of only spirals and only ellipticals, we start to get some hints. So, as the stellar populations age and become redder, NO new baby stars are added and the UV colour goes red.
There’s the parsec, a historical (but still used) unit of distance that was famously mis-used as a time in Star Wars.
It may be that, for some of the galaxies where there are clearly more details to flush out, we will ask for a few more classifications per galaxy.
This includes not just the recent meeting highlighting the importance of galaxy morphology in the era of large surveys at the Royal Astronomical Society and the upcoming ZooCon in Oxford and Galaxy Zoo meeting in Sydney, but also several more general conferences, including the 222nd American Astronomical Society meeting and the upcoming UK National Astronomy Meeting.
Why do some spiral galaxies have clearly defined spiral arms and others have flocculent structure that barely seems to hold together? New stars tend to form along the spiral arms, whereas older stars have time to spread out into more uniform orbits.
At a wavelength of 21 centimeters you can detect neutral Hydrogen, which provides raw material for the cooling and condensation of gas into cold, dense molecular clouds that form stars in their densest pockets. They’re rare in the local Universe, but how rare do we think they were billions of years ago, at the epoch we’re looking back to with Hubble? We understand quite a lot of it given that we are such a tiny part of it, but what we know is dwarfed by what we don’t.
Anyway, we made use of about 40% of the survey which is already complete, and which covers about 25% of the area of the sky in which the Galaxy Zoo galaxies are found (the Sloan Digital Sky Survey Legacy Area). Many spiral galaxies have a lot of atomic hydrogen (with perhaps as much as 10 times as much mass in hydrogen as in stars!), while a typical elliptical galaxy has very little atomic gas, and so cannot form lots of new stars.
The bar does this by driving the gas to the centre of the galaxy where it gets denser, turns into molecular hydrogen and from that stars (but only in the centre). I have been meaning for a while to make a new version of the Hubble tuning fork based on the type of images which were used in Galaxy Zoo 1 and 2 (OK the prettiest ones I could find – these are not typical at all).
You can see the halo quite well in the above image of the Sombrero Galaxy, which is a spiral seen almost edge-on. The stars orbit around the centre of mass of the galaxy in a more random way – their orbits are not constrained to a disk shape. It is thought that many irregulars were once ellipticals or spirals and have been distorted by interactions or collisions with other galaxies. What with the first Zoo 2 paper being submitted and a few other distractions as well it’s been a very busy week for her. The blue spiral arms in the galaxy pictured below, for example, mark sites of recent star formation. As this paper uses only Zoo 1 data, we just selected the roundest spirals assuming that this would get rid of those pesky edge-on systems; we also insist that Zooites were able to identify a direction to the spiral arms. Once we find ourselves near the core of a cluster of galaxies, the number and fraction of red spirals drops dramatically. We might find that those in the densest environments were redder than their (still quite red) counterparts further out, for example. When in the fat cells cannot see the result in the third set of serious condition is ergonomic style pushes running shoes? Audio Program: Running can do an example say that this treatment of shin splints still using one tough disease total running tiring painful and in the magazines.
Okay a side effect I get not listed that is making it very hard to type this – is the shakes. The role of each SRC is to identify deaths reportable to the ARD program I will also share my point of views on this topic here .
People with 10-15 pounds to lose often do better with deficits around 200-300 calories per day and weight loss of no more than half a pound per week.
But if I workout, even for a short time, I’ll have energy to get everything done that I want to do. Because they are still forming at least some baby stars and they are extremely bright and so blue that they emit a LOT of ultraviolet light. We also know observationally that gas turns into stars according to a specific recipe, the Schmidt-Kennicutt law.
And there will probably be future CANDELS images from survey fields that are still being completed. So ultraviolet observations of a galaxy, which tend to pick out the new and bright stars, often highlight the spiral arms much more strongly than longer-wavelength observations, which see more light from older stars. Each wavelength you observe at provides a glimpse at a different targeted feature of a spiral galaxy.
How long will it take for it to dissipate under the harsh radiation of the bright, young stars near it? And not just on the edges: in some parts you can see galaxies through the middle of the nebula. The next generation of stars had some metals, but the Universe has been around long enough that those stars (even the lower-mass ones that live for a long time) are past their prime and a new generation, one with compositions generally like our Sun, are now in their heyday.
Adding some cuts on how face-on the galaxies are so that the bars can be identified, and to make sure the sample contains the same size galaxies right through it’s volume we ended up with 2090 galaxies with both atomic hydrogen detections and bar classifications from you guys. There is very little star formation going on in elliptical galaxies and so they usually appear reddish in colour: dominated by older, cooler stars. Irregular galaxies can have very high star formation rates and can contain a lot of dust and gas – often more than spiral galaxies. So whatever it is that is causing the spirals to turn red must be more likely in the outskirts of galaxy clusters, but relatively rare outside this particular environment. It is said that doing cardio fasted will burn more fat opposed to having food in your system and was weight loss smoothies without bananas reviews antonio san wondering if there are any citeable articles on this topic that show best weight loss exercise on elliptical fat plan week 5 results of it being true or false. Episode 159: Mental Challenges After Weight Loss S In this weeks episode of BariatricTV we have a Drop Zone Freak who can keep on walking. It wasn't easy getting the pin OUT of the socket but it was nearly impossible to get it back in! So even as the overall population of young stars declines, the galaxy is still blue in the UV. Basically that law says that in any dynamical time (the characteristic time scale of the gas disk), a small fraction (around 2%) of that gas turns into stars. Eventually, almost no gas is left and the originally blue spiral bursting with blue young stars has fewer and fewer young stars and so turns green and eventually red. There are also hints that their black holes are feeding, so it’s possible an energetic outburst from their central black holes heated and ejected their gas reservoir in a short episode. So, don’t worry, there will still be plenty of opportunities to classify galaxies as they were 10 billion years ago!
Finally it’s possible that as a galaxy interacts with its neighbours, a bar gets triggered and its gas gets stripped (ie.
We don’t see any connection between the properties of the red spiral and the environment they find themselves in.
Their star formation rate is dropping, which is why they have fewer and fewer young blue stars. If the blue ellipticals turn green and then red, they must do so quickly, or there would be far more green ellipticals. This image alone contains spiral galaxy insights big and small, near and far, from the very distant universe and right in our own backyard. Calculate your daily caloric needs based on your height, weight, age, gender, and activity level.
A That said, once I got the pin out I sprayed on the silicon-based lubricant (and even sprayed some inside the socket) then attempted to reassemble. With this in mind, we can explain the behaviour of ellipticals and spirals in terms of what happens to their gas. We’ll need to do more work to figure out which of these (or which combination of them) is the most important. But they have their gas reservoir, so they keep moving, moving not knowing that they’re already doomed. Who wants their weight loss program run by a mean When planning for the period after having a gastric bypass operation, you should keep in mind To learn more about complications of gastric bypass surgery, visit Risks.
A I was able to get the pin into one side of the pedal and that's when the fun really began. I conclusion I personally feel that if I am going to add cardio to my workout routine then I want to do whatever it takes to maximize the workouts benefits. You have to hold the arm and the pedal while pulling them toward the back of the machine AND, at the same time, have a buddy bang away at the pin to jam it back into place. Sometimes that squeaks too.Mike Tomasevic: Would you be able to add a photo showing where the weld was sanded down? A I also lubricated the rails (and wiped off the excess liquid) but I'm pretty sure the squeaking was coming from the pin inside the pedal. Just look right below the foot pedal for the bolt that goes through the pedal and the end of the arm the pedal connects to. There is a "square block" under its head that fits into a square hole in the pedal's frame.

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